ORCID Profile
0000-0002-3254-9044
Current Organisation
Swinburne University of Technology
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Research Topics
In Research Link Australia (RLA), "Research Topics" refer to ANZSRC FOR and SEO codes. These topics are either sourced from ANZSRC FOR and SEO codes listed in researchers' related grants or generated by a large language model (LLM) based on their publications.
Top 5 Research Topics
ANZSRC Field of Research (FoR)
Astronomical and Space Sciences | Cosmology and Extragalactic Astronomy | Astronomical and Space Instrumentation | Astronomy And Astrophysics | Galactic Astronomy | Stellar Astronomy and Planetary Systems | Photonics, Optoelectronics and Optical Communications | Astroparticle physics and particle cosmology | Astronomical sciences | Antenna Technology | Digital Systems | Cosmology and extragalactic astronomy | Communications Technologies | Psychology | Sensory Processes, Perception and Performance | Behavioural Ecology | Nuclear And Particle Physics | Optics And Opto-Electronic Physics
ANZSRC Socio-Economic Objective (SEO)
Expanding Knowledge in the Physical Sciences | Physical sciences | Expanding Knowledge in Technology | Scientific instrumentation | Expanding Knowledge in Engineering | Solar-photoelectric | Expanding Knowledge in Psychology and Cognitive Sciences | Integrated circuits and devices | Expanding Knowledge in the Information and Computing Sciences | Expanding Knowledge in the Biological Sciences |
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Publications
The Fourth Data Release of the Sloan Digital Sky Survey
Publisher: American Astronomical Society
Date: 2006
DOI: 10.1086/497917
The Size Evolution of Star-forming Galaxies since z ∼ 7 Using ZFOURGE
Publisher: American Astronomical Society
Date: 09-01-2017
Early Results from GLASS–JWST. XXI. Rapid Asembly of a Galaxy at z = 6.23 Revealed by Its C/O Abundance
Publisher: American Astronomical Society
Date: 07-2023
Abstract: The abundance of carbon relative to oxygen (C/O) is a promising probe of star formation history in the early universe, as the ratio changes with time due to production of these elements by different nucleosynthesis pathways. We present a measurement of log ( C / O ) = − 1.01 ± 0.12 (stat) ±0.15 (sys) in a z = 6.23 galaxy observed as part of the GLASS–JWST Early Release Science Program. Notably, we achieve good precision thanks to the detection of the rest-frame ultraviolet O iii ], C iii ], and C iv emission lines delivered by JWST/NIRSpec. The C/O abundance is ∼0.8 dex lower than the solar value and is consistent with the expected yield from core-collapse supernovae, indicating that longer-lived intermediate-mass stars have not fully contributed to carbon enrichment. This in turn implies rapid buildup of a young stellar population with age ≲100 Myr in a galaxy seen ∼900 Myr after the big bang. Our chemical abundance analysis is consistent with spectral energy distribution modeling of JWST/NIRCam photometric data, which indicates a current stellar mass log M * / M ☉ = 8.4 − 0.2 + 0.4 and specific star formation rate ≃20 Gyr −1 . These results showcase the value of chemical abundances and C/O in particular to study the earliest stages of galaxy assembly.
Dynamic Equilibrium Sets of the Atomic Content of Galaxies across Cosmic Time
Publisher: American Astronomical Society
Date: 27-11-2018
First cosmology results using Type Ia supernova from the Dark Energy Survey: simulations to correct supernova distance biases
Publisher: Oxford University Press (OUP)
Date: 19-02-2019
DOI: 10.1093/MNRAS/STZ463
Optical-mechanical operation of the F2T2 Filter: A tunable filter designed to search for First Light
Publisher: SPIE
Date: 12-07-2008
DOI: 10.1117/12.789692
FIELD: Automated emission line detection software for Subaru/FMOS near-infrared spectroscopy
Publisher: Oxford University Press (OUP)
Date: 23-12-2014
DOI: 10.1093/PASJ/PSU127
The GLASS-JWST Early Release Science Program. I. Survey Design and Release Plans
Publisher: American Astronomical Society
Date: 08-2022
Abstract: The GLASS-JWST Early Release Science (hereafter GLASS-JWST-ERS) Program will obtain and make publicly available the deepest extragalactic data of the ERS c aign. It is primarily designed to address two key science questions, namely, “what sources ionized the universe and when?” and “how do baryons cycle through galaxies?”, while also enabling a broad variety of first look scientific investigations. In primary mode, it will obtain NIRISS and NIRSpec spectroscopy of galaxies lensed by the foreground Hubble Frontier Field cluster, Abell 2744. In parallel, it will use NIRCam to observe two fields that are offset from the cluster center, where lensing magnification is negligible, and which can thus be effectively considered blank fields. In order to prepare the community for access to this unprecedented data, we describe the scientific rationale, the survey design (including target selection and observational setups), and present pre-commissioning estimates of the expected sensitivity. In addition, we describe the planned public releases of high-level data products, for use by the wider astronomical community.
GRBâ090426: the environment of a rest-frame 0.35-s gamma-ray burst at a redshift of 2.609
Publisher: Oxford University Press (OUP)
Date: 11-01-2010
A Low Global Star Formation Rate in the Rich Galaxy Cluster AC 114 at z=0.32
Publisher: American Astronomical Society
Date: 10-03-2001
DOI: 10.1086/319459
Early Results from GLASS-JWST. XIV. A Spectroscopically Confirmed Protocluster 650 Million Years after the Big Bang
Publisher: American Astronomical Society
Date: 04-2023
Abstract: We present the spectroscopic confirmation of a protocluster at z = 7.88 behind the galaxy cluster Abell 2744 (hereafter A2744-z7p9OD). Using JWST NIRSpec, we find seven galaxies within a projected radius of 60 kpc. Although the galaxies reside in an overdensity around ≳20× greater than a random volume, they do not show strong Ly α emission. We place 2 σ upper limits on the rest-frame equivalent width –28 Å. Based on the tight upper limits to the Ly α emission, we constrain the volume-averaged neutral fraction of hydrogen in the intergalactic medium to be x HI 0.45 (68% C i ). Using an empirical M UV – M halo relation for in idual galaxies, we estimate that the total halo mass of the system is ≳4 × 10 11 M ⊙ . Likewise, the line-of-sight velocity dispersion is estimated to be 1100 ± 200 km s −1 . Using an empirical relation, we estimate the present-day halo mass of A2744-z7p9OD to be ∼2 × 10 15 M ⊙ , comparable to the Coma cluster. A2744-z7p9OD is the highest redshift spectroscopically confirmed protocluster to date, demonstrating the power of JWST to investigate the connection between dark-matter halo assembly and galaxy formation at very early times with medium-deep observations at hr total exposure time. Follow-up spectroscopy of the remaining photometric candidates of the overdensity will further refine the features of this system and help characterize the role of such overdensities in cosmic reionization.
A massive, quiescent galaxy at a redshift of 3.717
Publisher: Springer Science and Business Media LLC
Date: 04-2017
DOI: 10.1038/NATURE21680
Abstract: Finding massive galaxies that stopped forming stars in the early Universe presents an observational challenge because their rest-frame ultraviolet emission is negligible and they can only be reliably identified by extremely deep near-infrared surveys. These surveys have revealed the presence of massive, quiescent early-type galaxies appearing as early as redshift z ≈ 2, an epoch three billion years after the Big Bang. Their age and formation processes have now been explained by an improved generation of galaxy-formation models, in which they form rapidly at z ≈ 3-4, consistent with the typical masses and ages derived from their observations. Deeper surveys have reported evidence for populations of massive, quiescent galaxies at even higher redshifts and earlier times, using coarsely s led photometry. However, these early, massive, quiescent galaxies are not predicted by the latest generation of theoretical models. Here we report the spectroscopic confirmation of one such galaxy at redshift z = 3.717, with a stellar mass of 1.7 × 10
A low [CII]/[NII] ratio in the center of a massive galaxy at z = 3.7: Evidence for a transition to quiescence at high redshift? (Corrigendum)
Publisher: EDP Sciences
Date: 06-2021
ZFIRE
Publisher: American Astronomical Society
Date: 05-01-2017
Early Results from GLASS-JWST. XV. Properties of the Faintest Red Sources in the NIRCAM Deep Fields
Publisher: American Astronomical Society
Date: 04-2023
Abstract: We present a first look at the reddest 2–5 μ m sources found in deep images from the GLASS Early Release Science program. We undertake a general search, i.e., not looking for any particular spectral signatures, for sources detected only in bands redder than is reachable with the Hubble Space Telescope, and which would likely not have been identified in pre-JWST surveys. We search for sources down to AB ∼27 (corresponding to σ detection threshold) in any of the F200W to F444W filters, with a magnitude excess relative to F090W to F150W bands. Fainter than F444W we find 56 such sources of which 37 have reasonably constrained spectral energy distributions to which we can fit photometric redshifts. We find the majority of this population (∼65%) as 2 z 6 star-forming low-attenuation galaxies that are faint at rest-frame ultraviolet-optical wavelengths, have stellar masses 10 8.5 –10 9.5 M ⊙ , and have observed fluxes at μ m boosted by a combination of the Balmer break and emission lines. The typical implied rest equivalent widths are ∼200 Å with some extreme objects up to ∼1000 Å. This is in contrast with brighter magnitudes where the red sources tend to be z 3 quiescent galaxies and dusty star-forming objects. Our general selection criteria for red sources allow us to independently identify other phenomena as erse as extremely low-mass (∼10 8 M ⊙ ) quiescent galaxies at z 1, recovering recently identified z 11 galaxies and a very cool brown dwarf.
Dependence of star formation activity on stellar mass and environment from the Redshift One LDSS-3 Emission line Survey
Publisher: Oxford University Press (OUP)
Date: 17-11-2011
The Hubble Space Telescope Medium Deep Survey with the Wide Field and Planetary Camera. 1: Methodology and results on the field near 3C 273
Publisher: American Astronomical Society
Date: 12-1994
DOI: 10.1086/174976
Gnosis: The first instrument to use fiber bragg gratings for oh suppression
Publisher: American Astronomical Society
Date: 16-01-2013
Measurement of the star formation rate from Hα in field galaxies at z=1
Publisher: Oxford University Press (OUP)
Date: 11-07-1999
Search for new phenomena in photon + jet events collected in proton–proton collisions at
Publisher: Elsevier BV
Date: 2014
ZFIRE: using Hα equivalent widths to investigate the in situ initial mass function at z ̃ 2
Publisher: Oxford University Press (OUP)
Date: 14-03-2017
DOI: 10.1093/MNRAS/STX605
Low angular momentum in clumpy, turbulent disk galaxies
Publisher: American Astronomical Society
Date: 14-12-2015
Highly cited papers in dental medicine based on essential science indicators
Publisher: National Library of Serbia
Date: 2021
Abstract: Introduction/Objective. Essential Science Indicators (ESI) Highly Cited Papers (HCPs) refer to the most influential scientific articles and breakthrough research within a research field in the past decade. This study aimed to identify the characteristics of ESI HCPs in the subject category Dentistry, Oral Surgery and Medicine, to recognize authors, institutions and countries of origin, and determine research trends that attracted the most scientific interest in dentistry. Methods. A descriptive analysis of bibliographic data, network extraction and visualization were completed. Furthermore, analyzed ESI HCPs were classified according to a field of interest, main research domain, type of study, and level of evidence. Results. The set of 185 dental HCPs was published in 42 journals from 2010 to 2020, with an average number of 211.7 citations per paper. Nearly half of HCPs were issued by the Journal of Dental Research, Dental Materials, and Journal of Clinical Periodontology. There were 765 authors affiliated with 351 institutions from 42 countries. The most productive institutions were the University of Hong Kong, the University of Michigan, and the University of Bern. The United States of America contributed with the highest number of publications, followed by China, and the United Kingdom. Dental materials, dental implantology, periodontology, and oral and maxillofacial surgery represented areas of significant interest within this subject category. The highest proportion of HCPs were narrative and systematic reviews, expert opinions, consensus reports, and in vitro ?r lab studies. Conclusion. Results obtained from this study can provide valuable information for researchers to better identify present and future hotspots in dental research.
Suppression of the near-infrared OH night-sky lines with fibre Bragg gratings - first results
Publisher: Oxford University Press (OUP)
Date: 17-08-2012
A Tale of Two Clusters: An Analysis of Gas-phase Metallicity and Nebular Gas Conditions in Proto-cluster Galaxies at z ∼ 2
Publisher: American Astronomical Society
Date: 30-09-2019
MOSEL Survey: Tracking the Growth of Massive Galaxies at 2 < z < 4 Using Kinematics and the IllustrisTNG Simulation
Publisher: American Astronomical Society
Date: 09-04-2020
The SAMI Galaxy Survey: instrument specification and target selection
Publisher: Oxford University Press (OUP)
Date: 13-01-2015
Cosmological time dilation using type Ia supernovae as clocks
Publisher: Elsevier BV
Date: 11-1996
Deep Optical Imaging of the Bright Seyfert Galaxy NGC 5548: A Long, Very Low Surface Brightness Tail
Publisher: American Astronomical Society
Date: 07-1998
DOI: 10.1086/300395
Early Results from GLASS-JWST. XVI. Discovering a Bluer z ∼ 4–7 Universe through UV Slopes
Publisher: American Astronomical Society
Date: 04-2023
Abstract: We use the GLASS-JWST Early Release Science NIRCam parallel observations to provide a first view of the UV continuum properties of NIRCam/F444W selected galaxies at 4 z 7. By combining multiwavelength NIRCam observations, we constrain the UV continuum slope for a s le of 401 galaxies with stringent quality controls. We find that % of the galaxies are blue star-forming galaxies with very low levels of dust ( Av β ∼ 0.01 ± 0.33). We find no statistically significant correlation for UV slope with redshift or UV magnitude. However, we find that in general galaxies at higher redshifts and fainter UV magnitudes have steeper UV slopes. We find a statistically significant correlation for UV slope with stellar mass, with galaxies with higher stellar mass showing shallower UV slopes. In idual fits to some of our galaxies reach the bluest UV slopes of β ∼ −3.1 allowed by stellar population models used in this analysis. Therefore, it is likely that stellar population models with a higher amount of Lyman continuum leakage, active galactic nucleus effects, and/or Population III contributions are required to accurately reproduce the rest-UV and optical properties of some of our bluest galaxies. This dust-free early view confirms that our current cosmological understanding of gradual mass + dust buildup of galaxies with cosmic time is largely accurate to describe the ∼0.7–1.5 Gyr age window of the universe. The abundance of a large population of UV faint dust-poor systems may point to a dominance of low-mass galaxies at z 6 playing a vital role in cosmic reionization.
THE HOST GALAXIES OFSWIFTDARK GAMMA-RAY BURSTS: OBSERVATIONAL CONSTRAINTS ON HIGHLY OBSCURED AND VERY HIGH REDSHIFT GRBs
Publisher: American Astronomical Society
Date: 30-10-2009
Cosmic Star Formation History and Its Dependence on Galaxy Stellar Mass
Publisher: American Astronomical Society
Date: 03-01-2005
DOI: 10.1086/427937
The Sloan Digital Sky Surveyu-band Galaxy Survey: luminosity functions and evolution
Publisher: Oxford University Press (OUP)
Date: 04-2005
OzDES multi-object fibre spectroscopy for the Dark Energy Survey: results and second data release
Publisher: Oxford University Press (OUP)
Date: 30-05-3202
Abstract: We present a description of the Australian Dark Energy Survey (OzDES) and summarize the results from its 6 years of operations. Using the 2dF fibre positioner and AAOmega spectrograph on the 3.9-m Anglo-Australian Telescope, OzDES has monitored 771 active galactic nuclei, classified hundreds of supernovae, and obtained redshifts for thousands of galaxies that hosted a transient within the 10 deep fields of the Dark Energy Survey. We also present the second OzDES data release, containing the redshifts of almost 30 000 sources, some as faint as rAB = 24 mag, and 375 000 in idual spectra. These data, in combination with the time-series photometry from the Dark Energy Survey, will be used to measure the expansion history of the Universe out to z ∼ 1.2 and the masses of hundreds of black holes out to z ∼ 4. OzDES is a template for future surveys that combine simultaneous monitoring of targets with wide-field imaging cameras and wide-field multi-object spectrographs.
Testing gravity using galaxy-galaxy lensing and clustering amplitudes in KiDS-1000, BOSS, and 2dFLenS
Publisher: EDP Sciences
Date: 10-2020
DOI: 10.1051/0004-6361/202038505
Abstract: The physics of gravity on cosmological scales affects both the rate of assembly of large-scale structure and the gravitational lensing of background light through this cosmic web. By comparing the litude of these different observational signatures, we can construct tests that can distinguish general relativity from its potential modifications. We used the latest weak gravitational lensing dataset from the Kilo-Degree Survey, KiDS-1000, in conjunction with overlapping galaxy spectroscopic redshift surveys, BOSS and 2dFLenS, to perform the most precise existing litude-ratio test. We measured the associated E G statistic with 15 − 20% errors in five Δ z = 0.1 tomographic redshift bins in the range 0.2 z 0.7 on projected scales up to 100 h −1 Mpc. The scale-independence and redshift-dependence of these measurements are consistent with the theoretical expectation of general relativity in a Universe with matter density Ω m = 0.27 ± 0.04. We demonstrate that our results are robust against different analysis choices, including schemes for correcting the effects of source photometric redshift errors, and we compare the performance of angular and projected galaxy-galaxy lensing statistics.
An imaging K-band survey – II. The redshift survey and galaxy evolution in the infrared
Publisher: Oxford University Press (OUP)
Date: 07-1995
The GLARE Survey - II. Faint z ~ 6 Lyα line emitters in the HUDF
Publisher: Oxford University Press (OUP)
Date: 04-2007
The FourStar Galaxy Evolution Survey (ZFOURGE): Ultraviolet to Far-infrared Catalogs, Medium-bandwidth Photometric Redshifts with Improved Accuracy, Stellar Masses, and Confirmation of Quiescent Galaxies to z ̃ 3.5
Publisher: American Astronomical Society
Date: 10-10-2016
A low [CII]/[NII] ratio in the center of a massive galaxy at z = 3.7: Evidence for a transition to quiescence at high redshift?
Publisher: EDP Sciences
Date: 02-2021
DOI: 10.1051/0004-6361/201936460
Abstract: Understanding the process of quenching is one of the major open questions in galaxy evolution and crucial insights may be obtained by studying quenched galaxies at high redshifts at epochs when the Universe and the galaxies were younger and simpler to model. However, establishing the degree of quiescence in high-redshift galaxies is a challenging task. One notable ex le is Hyde, a recently discovered galaxy at z spec = 3.709. Equally as compact ( r 1/2 ∼ 0.5 kpc) and massive ( M * ∼ 10 11 M ⊙ ) as its quenched neighbor Jekyll, it is also extremely obscured yet only moderately luminous in the sub-millimeter. Panchromatic modeling has suggested it could be the first galaxy found in transition to quenching at z 3, however, the data are also consistent with a broad range of star-formation activity, from fully quenched to moderate star-formation rates (SFR) in the lower scatter of the galaxy main-sequence. Here, we describe Atacama Large Millimeter Array observations of the [C II ] 157 μ m and [N II ] 205 μ m far-infrared emission lines. The [C II ] emission within the half-light radius is dominated by ionized gas, while the outskirts are dominated by photo-dissociation regions or neutral gas. This suggests that the ionization in the center is not primarily powered by ongoing star formation, and is instead coming from remnant stellar populations formed in an older burst or from a moderate active galactic nucleus . Accounting for this information in the multi-wavelength modeling provides a tighter constraint on the star formation rate of SFR = 50 −18 +24 M ⊙ yr −1 yr −1 . This rules out fully quenched solutions and favors SFRs more than factor of two lower than expected for a main-sequence galaxy, confirming the nature of Hyde as a transition galaxy. These results suggest that quenching happens from inside-out and starts before the galaxy expels or consumes all its gas reservoirs. Similar observations of a s le of massive and obscured galaxies would determine whether this is an isolated case or the norm for quenching at high redshift.
KOALA: A wide-field, 1000 element integral-field unit for the Anglo-Australian Telescope
Publisher: SPIE
Date: 24-09-2012
DOI: 10.1117/12.925812
A study of selection methods for Hα-emitting galaxies at z ∼ 1.3 for the Subaru/FMOS galaxy redshift survey for cosmology (FastSound)
Publisher: Oxford University Press (OUP)
Date: 04-2014
DOI: 10.1093/PASJ/PSU022
Rapidly evolving transients in the Dark Energy Survey
Publisher: Oxford University Press (OUP)
Date: 29-08-2018
The WiggleZ Dark Energy Survey: measuring the cosmic growth rate with the two-point galaxy correlation function
Publisher: Oxford University Press (OUP)
Date: 07-02-2013
DOI: 10.1093/MNRAS/STS608
The WiggleZ Dark Energy Survey: Galaxy Evolution at 0.25 <= z <= 0.75 Using the Second Red-Sequence Cluster Survey
Publisher: American Astronomical Society
Date: 17-02-2012
Oral Abstracts
Publisher: Oxford University Press (OUP)
Date: 07-2016
DOI: 10.1111/IJPP.12278
The Hawaii+Anglo-Australian Observatory K-Band Galaxy Redshift Survey. I. The Local K-Band Luminosity Function
Publisher: American Astronomical Society
Date: 10-02-2003
DOI: 10.1086/345619
Hubble Space TelescopeImaging of the CFRS and LDSS Redshift Surveys. II. Structural Parameters and the Evolution of Disk Galaxies toz∼ 1
Publisher: American Astronomical Society
Date: 10-06-1998
DOI: 10.1086/305713
Combined search for the Standard Model Higgs boson using up to 4.9 fb−1 of pp collision data at <
Publisher: Elsevier BV
Date: 03-2012
Redshift distributions of galaxies in the Dark Energy Survey Science Verification shear catalogue and implications for weak lensing
Publisher: American Physical Society (APS)
Date: 30-08-2016
Science programs for a 2-m class telescope at dome C, antarctica: PILOT, the pathfinder for an International Large Optical Telescope
Publisher: Cambridge University Press (CUP)
Date: 2005
DOI: 10.1071/AS04077
Abstract: The cold, dry, and stable air above the summits of the Antarctic plateau provides the best ground-based observing conditions from optical to sub-millimetre wavelengths to be found on the Earth. Pathfinder for an International Large Optical Telescope (PILOT) is a proposed 2 m telescope, to be built at Dome C in Antarctica, able to exploit these conditions for conducting astronomy at optical and infrared wavelengths. While PILOT is intended as a pathfinder towards the construction of future grand-design facilities, it will also be able to undertake a range of fundamental science investigations in its own right. This paper provides the performance specifications for PILOT, including its instrumentation. It then describes the kinds of projects that it could best conduct. These range from planetary science to the search for other solar systems, from star formation within the Galaxy to the star formation history of the Universe, and from gravitational lensing caused by exo-planets to that produced by the cosmic web of dark matter. PILOT would be particularly powerful for wide-field imaging at infrared wavelengths, achieving near diffraction-limited performance with simple tip–tilt wavefront correction. PILOT would also be capable of near diffraction-limited performance in the optical wavebands, as well be able to open new wavebands for regular ground-based observation, in the mid-IR from 17 to 40 μm and in the sub-millimetre at 200 μm.
Automatic Redshift Determination by Use of Principal Component Analysis. I. Fundamentals
Publisher: American Astronomical Society
Date: 1998
DOI: 10.1086/305039
The Gigaparsec WiggleZ simulations: characterizing scale-dependant bias and associated systematics in growth of structure measurements
Publisher: Oxford University Press (OUP)
Date: 24-03-2015
DOI: 10.1093/MNRAS/STV314
Detection of the Baryon Acoustic Peak in the Large‐Scale Correlation Function of SDSS Luminous Red Galaxies
Publisher: American Astronomical Society
Date: 10-11-2005
DOI: 10.1086/466512
K-band Imaging of the Nearby Clumpy, Turbulent Disk Galaxy DYNAMO G04-1
Publisher: American Astronomical Society
Date: 02-2022
Abstract: We present a case study of the stellar clumps in G04-1—a clumpy, turbulent disk galaxy located at z = 0.13—from the DYnamics of Newly-Assembled Massive Objects s le, using adaptive optics-enabled K -band imaging (∼2.25 kpc arcsec −1 ) with Keck-NIRC2. We identify 15 stellar clumps in G04-1 with a range of masses from 3.6 × 10 6 –2.7 × 10 8 M ⊙ , and a median mass of ∼ 2.9 × 10 7 M ⊙ . Note that these masses decrease by about half when we apply a light correction for the underlying stellar disk. A majority (12 of 15) of the clumps observed in the K P -band imaging have associated components in H α maps (∼2.75 kpc arcsec −1 R clump ∼ 500 pc) and appear colocated ( Δ x ¯ ∼ 0 .″ 1 ). Using Hubble Space Telescope observations from the Wide Field Camera on the Advanced Camera for Surveys, with the F336W and F467M filters, we also find evidence of radial trends in the stellar properties of the clumps: the clumps closer to the center of G04-1 are more massive (consistent with observations in high- z systems) and appear more red, suggesting they may be more evolved. Using our high-resolution data, we construct a star-forming main sequence for G04-1 in terms of spatially resolved quantities, and find that all regions (both clump and intraclump) within the galaxy are experiencing an enhanced mode of star formation routinely observed in galaxies at high- z . In comparison to recent simulations, our observations of a number of clumps with masses of 10 7 –10 8 M ⊙ are not consistent with strong radiative feedback in this galaxy.
DES science portal: Computing photometric redshifts
Publisher: Elsevier BV
Date: 10-2018
Early Results from GLASS-JWST. IV. Spatially Resolved Metallicity in a Low-mass z ∼ 3 Galaxy with NIRISS*
Publisher: American Astronomical Society
Date: 10-2022
Abstract: We report the first gas-phase metallicity map of a distant galaxy measured with the James Webb Space Telescope (JWST). We use the NIRISS slitless spectroscopy acquired by the GLASS Early Release Science program to spatially resolve the rest-frame optical nebular emission lines in a gravitationally lensed galaxy at z = 3.06 behind the A2744 galaxy cluster. This galaxy (dubbed GLASS-Zgrad1) has stellar mass ∼10 8.6 M ⊙ , instantaneous star formation rate ∼8.6 M ⊙ yr −1 (both corrected for lensing magnification), and global metallicity one-fourth solar. From its emission-line maps ([O iii ], H β , H γ , [Ne iii ], and [O ii ]), we derive its spatial distribution of gas-phase metallicity using a well-established forward-modeling Bayesian inference method. The exquisite resolution and sensitivity of JWST/NIRISS, combined with lensing magnification, enable us to resolve this z ∼ 3 dwarf galaxy in ≳50 resolution elements with sufficient signal, an analysis hitherto not possible. We find that the radial metallicity gradient of GLASS-Zgrad1 is strongly inverted (i.e., positive): Δ log ( O / H ) / Δ r = 0.165 ± 0.023 dex kpc −1 . This measurement is robust at ≳ 4 − σ confidence level against known systematics. This positive gradient may be due to tidal torques induced by a massive nearby (∼15 kpc projected) galaxy, which can cause inflows of metal-poor gas into the central regions of GLASS-Zgrad1. These first results showcase the power of JWST wide-field slitless spectroscopic modes to resolve the mass assembly and chemical enrichment of low-mass galaxies in and beyond the peak epoch of cosmic star formation ( z ≳ 2). Reaching masses ≲ 10 9 M ⊙ at these redshifts is especially valuable to constrain the effects of galactic feedback and environment and is possible only with JWST’s new capabilities.
Early Results from GLASS-JWST. X. Rest-frame UV-optical Properties of Galaxies at 7 < z < 9
Publisher: American Astronomical Society
Date: 2023
Abstract: We present the first James Webb Space Telescope/NIRCam-led determination of 7 z 9 galaxy properties based on broadband imaging from 0.8 to 5 μ m as part of the GLASS-JWST Early Release Science program. This is the deepest data set acquired at these wavelengths to date, with an angular resolution ≲0.″14. We robustly identify 13 galaxies with signal-to-noise ratio ≳ 8 in F444W from 8 arcmin 2 of data at m AB ≤ 28 from a combination of dropout and photometric redshift selection. From simulated data modeling, we estimate the dropout s le purity to be ≳90%. We find that the number density of these F444W-selected sources is broadly consistent with expectations from the UV luminosity function determined from Hubble Space Telescope data. We characterize galaxy physical properties using a Bayesian spectral energy distribution fitting method, finding a median stellar mass of 10 8.5 M ⊙ and age 140 Myr, indicating they started ionizing their surroundings at redshift z 9.5. Their star formation main sequence is consistent with predictions from simulations. Lastly, we introduce an analytical framework to constrain main-sequence evolution at z 7 based on galaxy ages and basic assumptions, through which we find results consistent with expectations from cosmological simulations. While this work only gives a glimpse of the properties of typical galaxies that are thought to drive the reionization of the universe, it clearly shows the potential of JWST to unveil unprecedented details of galaxy formation in the first billion years.
Introducing the FLAMINGOS-2 Split-K Medium-band Filters: The Impact on Photometric Selection of High-z Galaxies in the FENIKS-pilot survey
Publisher: American Astronomical Society
Date: 03-11-2018
Abstract: Deep near-infrared photometric surveys are efficient in identifying high-redshift galaxies, however, they can be prone to systematic errors in photometric redshift. This is particularly salient when there is limited s ling of key spectral features of a galaxy’s spectral energy distribution (SED), such as for quiescent galaxies where the expected age-sensitive Balmer/4000 Å break enters the K -band at z 4. With single-filter s ling of this spectral feature, degeneracies between SED models and redshift emerge. A potential solution to this comes from splitting the K band into multiple filters. We use simulations to show an optimal solution is to add two medium-band filters, K blue ( λ cen = 2.06 μ m, Δ λ = 0.25 μ m) and K red ( λ cen = 2.31 μ m, Δ λ = 0.27 μ m), that are complementary to the existing K s filter. We test the impact of the K -band filters with simulated catalogs comprised of galaxies with varying ages and signal-to-noise. The results suggest that the K -band filters do improve photometric redshift constraints on z 4 quiescent galaxies, increasing precision and reducing outliers by up to 90%. We find that the impact from the K -band filters depends on the signal-to-noise, the redshift, and the SED of the galaxy. The filters we designed were built and used to conduct a pilot of the FLAMINGOS-2 Extragalactic Near-Infrared K -band Split survey. While no new z 4 quiescent galaxies are identified in the limited area pilot, the K blue and K red filters indicate strong Balmer/4000 Å breaks in existing candidates. Additionally, we identify galaxies with strong nebular emission lines, for which the K -band filters increase photometric redshift precision and in some cases indicate extreme star formation.
DYNAMO – I. A sample of Hα-luminous galaxies with resolved kinematics
Publisher: Oxford University Press (OUP)
Date: 13-11-2013
Radio galaxies in ZFOURGE/NMBS
Publisher: Oxford University Press (OUP)
Date: 25-11-0088
Measuring the Cosmic Evolution of Dark Energy with Baryonic Oscillations in the Galaxy Power Spectrum
Publisher: American Astronomical Society
Date: 20-09-2005
DOI: 10.1086/432497
Anglo-Australian Telescope Imaging and Microslit Spectroscopy in the Southern Hubble Deep Field
Publisher: American Astronomical Society
Date: 05-2006
DOI: 10.1086/501011
A Morphological Catalog of Galaxies in the Hubble deep Field
Publisher: American Astronomical Society
Date: 08-1996
DOI: 10.1086/118020
The 2dF Galaxy Redshift Survey: spectral types and luminosity functions
Publisher: Oxford University Press (OUP)
Date: 19-09-1999
The Gemini Deep Deep Survey. I. Introduction to the Survey, Catalogs, and Composite Spectra
Publisher: American Astronomical Society
Date: 05-2004
DOI: 10.1086/383557
GNOSIS: A novel near-infrared OH suppression unit at the AAT
Publisher: SPIE
Date: 24-09-2012
DOI: 10.1117/12.926483
Selection and Photometric Properties of K+A Galaxies
Publisher: American Astronomical Society
Date: 10-02-2004
DOI: 10.1086/380601
The WiggleZ Dark Energy Survey: final data release and the metallicity of UV-luminous galaxies
Publisher: Oxford University Press (OUP)
Date: 21-11-2018
OzDES multifibre spectroscopy for the Dark Energy Survey: 3-yr results and first data release
Publisher: Oxford University Press (OUP)
Date: 26-07-2017
The KMOS Redshift One Spectroscopic Survey (KROSS): The origin of disc turbulence in z≈1 star-forming galaxies
Publisher: Oxford University Press (OUP)
Date: 23-11-2018
The WiggleZ Dark Energy Survey: Small-scale clustering of Lyman-break galaxies at z < 1
Publisher: Oxford University Press (OUP)
Date: 05-2009
The WiggleZ dark energy survey
Publisher: Oxford University Press (OUP)
Date: 10-2008
The Color Selection of Quasars from Redshifts 5 to 10: Cloning and Discovery
Publisher: American Astronomical Society
Date: 07-2005
DOI: 10.1086/430525
Galaxy bimodality versus stellar mass and environment
Publisher: Oxford University Press (OUP)
Date: 12-2006
Design of a multi-object high-throughput low-resolution fiber spectrograph for WFMOS
Publisher: SPIE
Date: 14-06-2006
DOI: 10.1117/12.672186
KiDS-1000 Cosmology: Multi-probe weak gravitational lensing and spectroscopic galaxy clustering constraints
Publisher: EDP Sciences
Date: 02-2021
DOI: 10.1051/0004-6361/202039063
Abstract: We present a joint cosmological analysis of weak gravitational lensing observations from the Kilo-Degree Survey (KiDS-1000), with redshift-space galaxy clustering observations from the Baryon Oscillation Spectroscopic Survey (BOSS) and galaxy-galaxy lensing observations from the overlap between KiDS-1000, BOSS, and the spectroscopic 2-degree Field Lensing Survey. This combination of large-scale structure probes breaks the degeneracies between cosmological parameters for in idual observables, resulting in a constraint on the structure growth parameter S 8 = σ 8 √(Ω m /0.3) = 0.766 −0.014 +0.020 , which has the same overall precision as that reported by the full-sky cosmic microwave background observations from Planck . The recovered S 8 litude is low, however, by 8.3 ± 2.6% relative to Planck . This result builds from a series of KiDS-1000 analyses where we validate our methodology with variable depth mock galaxy surveys, our lensing calibration with image simulations and null-tests, and our optical-to-near-infrared redshift calibration with multi-band mock catalogues and a spectroscopic-photometric clustering analysis. The systematic uncertainties identified by these analyses are folded through as nuisance parameters in our cosmological analysis. Inspecting the offset between the marginalised posterior distributions, we find that the S 8 -difference with Planck is driven by a tension in the matter fluctuation litude parameter, σ 8 . We quantify the level of agreement between the cosmic microwave background and our large-scale structure constraints using a series of different metrics, finding differences with a significance ranging between ∼3 σ , when considering the offset in S 8 , and ∼2 σ , when considering the full multi-dimensional parameter space.
The AST3-NIR camera for the Kunlun Infrared Sky Survey
Publisher: SPIE
Date: 09-08-2016
DOI: 10.1117/12.2233317
Are professional pharmacy services being offered for free in pharmacies? A feasibility study exploring the use of a time motion study in New Zealand
Publisher: JCFCorp SG PTE LTD
Date: 31-07-2021
DOI: 10.18549/PHARMPRACT.2021.3.2422
Abstract: Background: Pharmacists report to be providing patient-focused clinical services for which they receive no remuneration. Limited literature exists about unfunded services leading to difficulties in ascertaining an appropriate study design for such research. Objective: This study aims to assess the appropriateness of a proposed study design before launching a nationwide study to investigate the provision of unfunded patient care services. Methods: A multi-methods approach was utilised consisting of (1) continuous time motion study in community pharmacies (2) semi structured patient interviews (3) patient follow up (4) semi structured interviews with pharmacy owners/managers. All observations of unfunded patient care services were recorded, numerically coded and descriptively analysed. Semi structured interviews were audio recorded and transcribed verbatim. A semantic thematic analysis was carried out. Appropriateness of study design was dictated by the ability to characterise services and obtain patient perceptions. Results: Ten pharmacies took part in the feasibility study, across the city of Dunedin, New Zealand, representing a range of different practice settings and demographics. Ten patients were interviewed and six responded to follow up. Both pharmacy and patient recruitment proved challenging due to concerns around disruption to workflow and patient privacy. A continuous observation time motion study was found to be appropriate as it minimises disruption to workflow with no additional work required from the pharmacy teams. Conclusions: A continuous observation time motion study proved to be an appropriate method to investigate the provision of unfunded services on a national scale. The findings of the study suggest design changes such as length of observation time, increasing patient recruitment and additional patient questions to enhance the nationwide study.
Galaxy morphology to I=25 mag in the Hubble Deep Field
Publisher: Oxford University Press (OUP)
Date: 04-1996
Universal fitting formulae for baryon oscillation surveys
Publisher: Oxford University Press (OUP)
Date: 2006
Systematic Difference between Ionized and Molecular Gas Velocity Dispersions in z ∼ 1–2 Disks and Local Analogs
Publisher: American Astronomical Society
Date: 03-2021
Abstract: We compare the molecular and ionized gas velocity dispersions of nine nearby turbulent disks, analogs to high-redshift galaxies, from the DYNAMO s le using new Atacama Large Millimeter/submillimeter Array and GMOS/Gemini observations. We combine our s le with 12 galaxies at z ∼ 0.5–2.5 from the literature. We find that the resolved velocity dispersion is systematically lower by a factor 2.45 ± 0.38 for the molecular gas compared to the ionized gas, after correcting for thermal broadening. This offset is constant within the galaxy disks and indicates the coexistence of a thin molecular gas disk and a thick ionized one. This result has a direct impact on the Toomre Q and pressure derived in galaxies. We obtain pressures ∼0.22 dex lower on average when using the molecular gas velocity dispersion, σ 0,mol . We find that σ 0,mol increases with gas fraction and star formation rate. We also obtain an increase with redshift and show that the EAGLE and FIRE simulations overall overestimate σ 0,mol at high redshift. Our results suggest that efforts to compare the kinematics of gas using ionized gas as a proxy for the total gas may overestimate the velocity dispersion by a significant amount in galaxies at the peak of cosmic star formation. When using the molecular gas as a tracer, our s le is not consistent with predictions from star formation models with constant efficiency, even when including transport as a source of turbulence. Feedback models with variable star formation efficiency, ϵ ff , and/or feedback efficiency, p * / m * , better predict our observations.
The Fifth Data Release of the Sloan Digital Sky Survey
Publisher: American Astronomical Society
Date: 10-2007
DOI: 10.1086/518864
Robust cross-correlation-based measurement of clump sizes in galaxies
Publisher: American Astronomical Society
Date: 09-08-2017
The WiggleZ Dark Energy Survey: the growth rate of cosmic structure since redshift z=0.9
Publisher: Oxford University Press (OUP)
Date: 07-06-2011
A substantial population of massive quiescent galaxies at z ~ 4 from ZFOURGE
Publisher: American Astronomical Society
Date: 18-02-2014
MARZ: Manual and automatic redshifting software
Publisher: Elsevier BV
Date: 04-2016
All femtosecond optical pump and X-ray probe: holey-axicon for free electron lasers
Publisher: IOP Publishing
Date: 18-12-2020
The WiggleZ Dark Energy Survey: joint measurements of the expansion and growth history atz< 1
Publisher: Oxford University Press (OUP)
Date: 19-07-2012
The WiggleZ dark energy survey: The selection function and z = 0.6 galaxy power spectrum
Publisher: Oxford University Press (OUP)
Date: 05-2010
The stellar masses of ̃ 40 000 UV selected Galaxies from the WiggleZ survey at 0.3
Publisher:
Oxford University Press (OUP)
Date:
20-03-2013
DOI:
10.1093/MNRAS/STT320
Publisher: Oxford University Press (OUP)
Date: 20-03-2013
DOI: 10.1093/MNRAS/STT320
On the Dearth of Compact, Massive, Red Sequence Galaxies in the Local Universe
Publisher: American Astronomical Society
Date: 13-08-2010
Early Results from GLASS-JWST. XI. Stellar Masses and Mass-to-light Ratio of z > 7 Galaxies
Publisher: American Astronomical Society
Date: 2023
Abstract: We exploit James Webb Space Telescope (JWST) NIRCam observations from the GLASS-JWST-Early Release Science program to investigate galaxy stellar masses at z 7. We first show that JWST observations reduce the uncertainties on the stellar mass by a factor of at least 5–10, when compared with the highest-quality data sets available to date. We then study the UV mass-to-light ratio, finding that galaxies exhibit a a two orders of magnitude range of M / L UV values for a given luminosity, indicative of a broad variety of physical conditions and star formation histories. As a consequence, previous estimates of the cosmic stellar-mass density—based on an average correlation between UV luminosity and stellar mass—can be biased by as much as a factor of ∼6. Our first exploration demonstrates that JWST represents a new era in our understanding of stellar masses at z 7 and, therefore, of the growth of galaxies prior to cosmic reionization.
The WiggleZ Dark Energy Survey: improved distance measurements to z = 1 with reconstruction of the baryonic acoustic feature
Publisher: Oxford University Press (OUP)
Date: 31-05-2014
DOI: 10.1093/MNRAS/STU778
Angular momentum regulates H i gas content and H i central hole size in the discs of spirals
Publisher: Oxford University Press (OUP)
Date: 30-11-2019
Beyond UVJ: Color Selection of Galaxies in the JWST Era
Publisher: American Astronomical Society
Date: 02-2023
Abstract: We present a new rest-frame color–color selection method using synthetic u s − g s and g s − i s , ( ugi ) s colors to identify star-forming and quiescent galaxies. Our method is similar to the widely used U − V versus V − J ( UVJ ) diagram. However, UVJ suffers known systematics. Spectroscopic c aigns have shown that UVJ -selected quiescent s les at z ≳ 3 include ∼10%–30% contamination from galaxies with dust-obscured star formation and strong emission lines. Moreover, at z 3, UVJ colors are extrapolated because the rest-frame band shifts beyond the coverage of the deepest bandpasses at μ m (typically Spitzer/IRAC 4.5 μ m or future JWST/NIRCam observations). We demonstrate that ( ugi ) s offers improvements to UVJ at z 3, and can be applied to galaxies in the JWST era. We apply ( ugi ) s selection to galaxies at 0.5 z 6 from the (observed) 3D-HST and UltraVISTA catalogs, and to the (simulated) JAGUAR catalogs. We show that extrapolation can affect ( V − J ) 0 color by up to 1 mag, but changes ( g s − i s ) 0 color by ≤0.2 mag, even at z ≃ 6. While ( ugi ) s -selected quiescent s les are comparable to UVJ in completeness (both achieve ∼85%–90% at z = 3–3.5), ( ugi ) s reduces contamination in quiescent s les by nearly a factor of 2, from ≃35% to ≃17% at z = 3, and from ≃60% to ≃33% at z = 6. This leads to improvements in the true-to-false-positive ratio (TP/FP), where we find TP/FP ≳2.2 for ( ugi ) s at z ≃ 3.5 − 6, compared to TP/FP 1 for UVJ -selected s les. This indicates that contaminants will outnumber true quiescent galaxies in UVJ at these redshifts, while ( ugi ) s will provide higher-fidelity s les.
The WiggleZ Dark Energy Survey: High-resolution kinematics of luminous star-forming galaxies
Publisher: Oxford University Press (OUP)
Date: 19-09-2011
The WiggleZ Dark Energy Survey: Final data release and cosmological results
Publisher: American Physical Society (APS)
Date: 16-11-2012
Supernova host galaxies in the dark energy survey: I. Deep coadds, photometry, and stellar masses
Publisher: Oxford University Press (OUP)
Date: 19-05-2020
Abstract: The 5-yr Dark Energy Survey Supernova Programme (DES-SN) is one of the largest and deepest transient surveys to date in terms of volume and number of supernovae. Identifying and characterizing the host galaxies of transients plays a key role in their classification, the study of their formation mechanisms, and the cosmological analyses. To derive accurate host galaxy properties, we create depth-optimized coadds using single-epoch DES-SN images that are selected based on sky and atmospheric conditions. For each of the five DES-SN seasons, a separate coadd is made from the other four seasons such that each SN has a corresponding deep coadd with no contaminating SN emission. The coadds reach limiting magnitudes of order ∼27 in g band, and have a much smaller magnitude uncertainty than the previous DES-SN host templates, particularly for faint objects. We present the resulting multiband photometry of host galaxies for s les of spectroscopically confirmed type Ia (SNe Ia), core-collapse (CCSNe), and superluminous (SLSNe) as well as rapidly evolving transients (RETs) discovered by DES-SN. We derive host galaxy stellar masses and probabilistically compare stellar-mass distributions to s les from other surveys. We find that the DES spectroscopically confirmed s le of SNe Ia selects preferentially fewer high-mass hosts at high-redshift compared to other surveys, while at low redshift the distributions are consistent. DES CCSNe and SLSNe hosts are similar to other s les, while RET hosts are unlike the hosts of any other transients, although these differences have not been disentangled from selection effects.
Cambridge OH suppression instrument (COHSI): status after first commissioning run
Publisher: SPIE
Date: 21-08-1998
DOI: 10.1117/12.317329
Dark Energy Survey Year 1 results: cross-correlation redshifts – methods and systematics characterization
Publisher: Oxford University Press (OUP)
Date: 22-02-2018
DOI: 10.1093/MNRAS/STY466
The SAMI Galaxy Survey: Bayesian inference for gas disc kinematics using a hierarchical Gaussian mixture model
Publisher: Oxford University Press (OUP)
Date: 08-03-2019
DOI: 10.1093/MNRAS/STZ670
Abstract: We present a novel Bayesian method, referred to as blobby3d, to infer gas kinematics that mitigates the effects of beam smearing for observations using integral field spectroscopy. The method is robust for regularly rotating galaxies despite substructure in the gas distribution. Modelling the gas substructure within the disc is achieved by using a hierarchical Gaussian mixture model. To account for beam smearing effects, we construct a modelled cube that is then convolved per wavelength slice by the seeing, before calculating the likelihood function. We show that our method can model complex gas substructure including clumps and spiral arms. We also show that kinematic asymmetries can be observed after beam smearing for regularly rotating galaxies with asymmetries only introduced in the spatial distribution of the gas. We present findings for our method applied to a s le of 20 star-forming galaxies from the SAMI Galaxy Survey. We estimate the global H α gas velocity dispersion for our s le to be in the range $\\bar{\\sigma }_v \\sim$[7, 30] km s−1. The relative difference between our approach and estimates using the single Gaussian component fits per spaxel is $\\Delta \\bar{\\sigma }_v / \\bar{\\sigma }_v = - 0.29 \\pm 0.18$ for the H α flux-weighted mean velocity dispersion.
Near-Infrared Photometry and Spectroscopy of L and T Dwarfs: The Effects of Temperature, Clouds, and Gravity
Publisher: American Astronomical Society
Date: 06-2004
DOI: 10.1086/420707
KiDS-450 + 2dFLenS: Cosmological parameter constraints from weak gravitational lensing tomography and overlapping redshift-space galaxy clustering
Publisher: Oxford University Press (OUP)
Date: 31-10-2018
Fundamental mass-spin-morphology relation of spiral galaxies
Publisher: American Astronomical Society
Date: 28-02-2014
Connecting Clump Sizes in Turbulent Disk Galaxies to Instability Theory
Publisher: American Astronomical Society
Date: 06-04-2017
DES meets Gaia: discovery of strongly lensed quasars from a multiplet search
Publisher: Oxford University Press (OUP)
Date: 04-06-2018
Superluminous supernovae from the Dark Energy Survey
Publisher: Oxford University Press (OUP)
Date: 21-05-2019
Abstract: We present a s le of 21 hydrogen-free superluminous supernovae (SLSNe-I) and one hydrogen-rich SLSN (SLSN-II) detected during the five-year Dark Energy Survey (DES). These SNe, located in the redshift range 0.220 & z & 1.998, represent the largest homogeneously selected s le of SLSN events at high redshift. We present the observed g, r, i, z light curves for these SNe, which we interpolate using Gaussian processes. The resulting light curves are analysed to determine the luminosity function of SLSNe-I, and their evolutionary time-scales. The DES SLSN-I s le significantly broadens the distribution of SLSN-I light-curve properties when combined with existing s les from the literature. We fit a magnetar model to our SLSNe, and find that this model alone is unable to replicate the behaviour of many of the bolometric light curves. We search the DES SLSN-I light curves for the presence of initial peaks prior to the main light-curve peak. Using a shock breakout model, our Monte Carlo search finds that 3 of our 14 events with pre-max data display such initial peaks. However, 10 events show no evidence for such peaks, in some cases down to an absolute magnitude of & −16, suggesting that such features are not ubiquitous to all SLSN-I events. We also identify a red pre-peak feature within the light curve of one SLSN, which is comparable to that observed within SN2018bsz.
ZFOURGE catalogue of AGN candidates: an enhancement of 160-μm-derived star formation rates in active galaxies to z = 3.2
Publisher: Oxford University Press (OUP)
Date: 22-01-2016
Early Results from GLASS-JWST. V: The First Rest-frame Optical Size–Luminosity Relation of Galaxies at z > 7
Publisher: American Astronomical Society
Date: 10-2022
Abstract: We present the first rest-frame optical size–luminosity relation of galaxies at z 7, using the NIRCam imaging data obtained by the GLASS James Webb Space Telescope Early Release Science (GLASS-JWST-ERS) program, providing the deepest extragalactic data of the ERS c aign. Our s le consists of 19 photometrically selected bright galaxies with m F444W ≤ 27.8 at 7 z 9 and m F444W 28.2 at z ∼ 9−15. We measure the size of the galaxies in five bands, from rest-frame optical (∼4800 Å) to the UV (∼1600 Å) based on the Sérsic model, and analyse the size–luminosity relation as a function of wavelength. Remarkably, the data quality of the NIRCam imaging is sufficient to probe the half-light radius r e down to ∼100 pc at z 7. Given the limited s le size and magnitude range, we first fix the slope to that observed for larger s les in rest-frame UV using Hubble Space Telescope s les. The median size r 0 at the reference luminosity M = −21 decreases slightly from rest-frame optical (600 ± 80 pc) to UV (450 ± 130 pc). We then refit the size–luminosity relation allowing the slope to vary. The slope is consistent with β ∼ 0.2 for all bands except F150W, where we find a marginally steeper slope of β = 0.53 ± 0.15. The steep UV slope is mainly driven by the smallest and faintest galaxies. If confirmed by larger s les, it implies that the UV size–luminosity relation breaks toward the faint end, as suggested by lensing studies.
Cold-mode accretion
Publisher: American Astronomical Society
Date: 18-07-2016
Imaging with diffractive axicons rapidly milled on sapphire by femtosecond laser ablation
Publisher: Springer Science and Business Media LLC
Date: 22-10-2021
Exploring the z = 3-4 massive galaxy population with ZFOURGE
Publisher: American Astronomical Society
Date: 20-05-2014
Scaling relations of star-forming regions: from kpc-sized clumps to H II regions
Publisher: Oxford University Press (OUP)
Date: 17-04-2012
An unusual high-redshift object discovered with the Hubble Space Telescope: peculiar starburst galaxy or new gravitational lens?
Publisher: Oxford University Press (OUP)
Date: 09-1994
L' and M' Photometry of Ultracool Dwarfs
Publisher: American Astronomical Society
Date: 06-2004
DOI: 10.1086/420709
Optical/Near‐Infrared Observations of GRO J1744−28
Publisher: American Astronomical Society
Date: 05-1997
DOI: 10.1086/303973
Early Results from GLASS-JWST. XVIII. A First Morphological Atlas of the 1 < z < 5 Universe in the Rest-frame Optical
Publisher: American Astronomical Society
Date: 05-2023
Abstract: We present a rest-frame optical morphological analysis of galaxies observed with the NIRCam imager on the James Webb Space Telescope (JWST) as part of the GLASS-JWST Early Release Science program. We select 388 sources at redshifts 0.8 z 5.4 and use the seven 0.9–5 μ m NIRCam filters to generate rest-frame gri composite color images, and conduct visual morphological classification. Compared to Hubble Space Telescope (HST)–based work we find a higher incidence of disks and bulges than expected at z 1.5, revealed by rest-frame optical imaging. We detect 123 clear disks (58 at z 1.5) of which 76 have bulges. No evolution of bulge fraction with redshift is evident: 61% at z 2 ( N = 110) versus 60% at z ≥ 2 ( N = 13). A stellar mass dependence is evident, with bulges visible in 80% of all disk galaxies with mass 9.5 M ⊙ ( N = 41) but only 52% at M 10 9.5 M ⊙ ( N = 82). We supplement visual morphologies with nonparametric measurements of Gini and asymmetry coefficients in the rest-frame i band. Our sources are more asymmetric than local galaxies, with slightly higher Gini values. When compared to high- z rest-frame ultraviolet measurements with HST, JWST shows more regular morphological types such as disks, bulges, and spiral arms at z 1.5, with smoother (i.e., lower Gini) and more symmetrical light distributions.
Early Results from GLASS-JWST. XX. Unveiling a Population of “Red Excess” Galaxies in Abell2744 and in the Coeval Field
Publisher: American Astronomical Society
Date: 05-2023
Abstract: We combine JWST/NIRCam imaging and MUSE data to characterize the properties of galaxies in different environmental conditions in the cluster Abell2744 ( z = 0.3064) and in its immediate surroundings. We investigate how galaxy colors, morphology, and star-forming fractions depend on wavelength and on different parameterizations of environment. Our most striking result is the discovery of a “red excess” population in F200W−F444W colors in both the cluster regions and the field. These galaxies have normal F115W−F150W colors but are up to 0.8 mag redder than red sequence galaxies in F200W−F444W. They also have rather blue rest-frame B − V colors. Galaxies in the field and at the cluster virial radius are overall characterized by redder colors, but galaxies with the largest color deviations are found in the field and in the cluster core. Several results suggest that mechanisms taking place in these regions might be more effective in producing these colors. Looking at their morphology, many cluster galaxies show signatures consistent with ram pressure stripping, while field galaxies have features resembling interactions and mergers. Our hypothesis is that these galaxies are characterized by dust-enshrouded star formation: a JWST/NIRSpec spectrum for one of the galaxies is dominated by a strong PAH at 3.3 μ m, suggestive of dust-obscured star formation. Larger spectroscopic s les are needed to understand whether the color excess is due exclusively to dust-obscured star formation, as well as the role of environment in triggering it.
Measurements of the Cosmological Parameters Ω and Λ from the First Seven Supernovae atz≥ 0.35
Publisher: American Astronomical Society
Date: 10-07-1997
DOI: 10.1086/304265
The local star formation rate density: assessing calibrations using [OII], H and UV luminosities
Publisher: Oxford University Press (OUP)
Date: 04-2010
The SAMI Galaxy Survey: the low-redshift stellar mass Tully–Fisher relation
Publisher: Oxford University Press (OUP)
Date: 19-07-2017
KiDS-1000 Cosmology: Constraints beyond flat ΛCDM
Publisher: EDP Sciences
Date: 05-2021
DOI: 10.1051/0004-6361/202039805
Abstract: We present constraints on extensions to the standard cosmological model of a spatially flat Universe governed by general relativity, a cosmological constant (Λ), and cold dark matter (CDM) by varying the spatial curvature Ω K , the sum of the neutrino masses ∑ m ν , the dark energy equation of state parameter w , and the Hu-Sawicki f ( R ) gravity f R 0 parameter. With the combined 3 × 2 pt measurements of cosmic shear from the Kilo-Degree Survey (KiDS-1000), galaxy clustering from the Baryon Oscillation Spectroscopic Survey (BOSS), and galaxy-galaxy lensing from the overlap between KiDS-1000, BOSS, and the spectroscopic 2-degree Field Lensing Survey, we find results that are fully consistent with a flat ΛCDM model with Ω K = 0.011 −0.057 +0.054 , ∑ m ν 1.76 eV (95% CL), and w = −0.99 −0.13 +0.11 . The f R 0 parameter is unconstrained in our fully non-linear f ( R ) cosmic shear analysis. Considering three different model selection criteria, we find no clear preference for either the fiducial flat ΛCDM model or any of the considered extensions. In addition to extensions to the flat ΛCDM parameter space, we also explore restrictions to common subsets of the flat ΛCDM parameter space by fixing the litude of the primordial power spectrum to the Planck best-fit value, as well as adding external data from supernovae and lensing of the cosmic microwave background (CMB). Neither the beyond-ΛCDM models nor the imposed restrictions explored in this analysis are able to resolve the ∼3 σ tension in S 8 between the 3 × 2 pt constraints and the Planck temperature and polarisation data, with the exception of w CDM, where the S 8 tension is resolved. The tension in the w CDM case persists, however, when considering the joint S 8 − w parameter space. The joint flat ΛCDM CMB lensing and 3 × 2 pt analysis is found to yield tight constraints on Ω m = 0.307 −0.013 +0.008 , σ 8 = 0.769 −0.010 +0.022 , and S 8 = 0.779 −0.013 +0.013 .
The sizes of massive quiescent and star-forming galaxies at z ∼ 4 with ZFOURGE and CANDELS
Publisher: American Astronomical Society
Date: 23-07-2015
Quantifying the Bimodal Color-Magnitude Distribution of Galaxies
Publisher: American Astronomical Society
Date: 10-01-2004
DOI: 10.1086/380092
Discovery of a Candidate Binary Supermassive Black Hole in a Periodic Quasar from Circumbinary Accretion Variability
Publisher: Oxford University Press (OUP)
Date: 10-10-2020
Abstract: Binary supermassive black holes (BSBHs) are expected to be a generic byproduct from hierarchical galaxy formation. The final coalescence of BSBHs is thought to be the loudest gravitational wave (GW) siren, yet no confirmed BSBH is known in the GW-dominated regime. While periodic quasars have been proposed as BSBH candidates, the physical origin of the periodicity has been largely uncertain. Here we report discovery of a periodicity (P=1607±7 days) at 99.95% significance (with a global p-value of ∼10−3 accounting for the look elsewhere effect) in the optical light curves of a redshift 1.53 quasar, SDSS J025214.67−002813.7. Combining archival Sloan Digital Sky Survey data with new, sensitive imaging from the Dark Energy Survey, the total ∼20-yr time baseline spans ∼4.6 cycles of the observed 4.4-yr (restframe 1.7-yr) periodicity. The light curves are best fit by a bursty model predicted by hydrodynamic simulations of circumbinary accretion disks. The periodicity is likely caused by accretion rate modulation by a milli-parsec BSBH emitting GWs, dynamically coupled to the circumbinary accretion disk. A bursty hydrodynamic variability model is statistically preferred over a smooth, sinusoidal model expected from relativistic Doppler boost, a kinematic effect proposed for PG1302−102. Furthermore, the frequency dependence of the variability litudes disfavors Doppler boost, lending independent support to the circumbinary accretion variability hypothesis. Given our detection rate of one BSBH candidate from circumbinary accretion variability out of 625 quasars, it suggests that future large, sensitive synoptic surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time may be able to detect hundreds to thousands of candidate BSBHs from circumbinary accretion with direct implications for Laser Interferometer Space Antenna.
Early Results from GLASS-JWST. III. Galaxy Candidates at z ∼9–15*
Publisher: American Astronomical Society
Date: 10-2022
Abstract: We present the results of a first search for galaxy candidates at z ∼ 9–15 on deep seven-band NIRCam imaging acquired as part of the GLASS-James Webb Space Telescope (JWST) Early Release Science Program on a flanking field of the Frontier Fields cluster A2744. Candidates are selected via two different renditions of the Lyman-break technique, isolating objects at z ∼ 9–11, and z ∼ 9–15, respectively, supplemented by photometric redshifts obtained with two independent codes. We find five color-selected candidates at z 9, plus one additional candidate with photometric redshift z phot ≥ 9. In particular, we identify two bright candidates at M UV ≃ −21 that are unambiguously placed at z ≃ 10.6 and z ≃ 12.2, respectively. The total number of galaxies discovered at z 9 is in line with the predictions of a nonevolving luminosity function. The two bright ones at z 10 are unexpected given the survey volume, although cosmic variance and small number statistics limits general conclusions. This first search demonstrates the unique power of JWST to discover galaxies at the high-redshift frontier. The candidates are ideal targets for spectroscopic follow-up in Cycle-2.
Microslit nod-shuffle spectroscopy: A technique for achieving very high densities of spectra
Publisher: IOP Publishing
Date: 02-2001
DOI: 10.1086/318625
A supernova at Z = 0.458 and implications for measuring the cosmological deceleration
Publisher: American Astronomical Society
Date: 02-1995
DOI: 10.1086/187756
KiDS+2dFLenS+GAMA: testing the cosmological model with the EG statistic
Publisher: Oxford University Press (OUP)
Date: 23-06-2018
MOSEL: Strong [Oiii] 5007 Å Emitting Galaxies at (3 < z < 4) from the ZFOURGE Survey
Publisher: American Astronomical Society
Date: 21-07-2020
The Dark Energy Survey: Data Release 1
Publisher: American Astronomical Society
Date: 26-11-2018
The Subaru FMOS galaxy redshift survey (FastSound). V. Intrinsic alignments of emission-line galaxies at z ∼ 1.4
Publisher: Oxford University Press (OUP)
Date: 14-04-2018
DOI: 10.1093/PASJ/PSY030
A high abundance of massive galaxies 3–6 billion years after the Big Bang
Publisher: Springer Science and Business Media LLC
Date: 07-2004
DOI: 10.1038/NATURE02667
The star formation history of the Hubble sequence: spatially resolved colour distributions of intermediate-redshift galaxies in the Hubble Deep Field
Publisher: Oxford University Press (OUP)
Date: 11-03-1999
The dynamics and distribution of angular momentum in HiZELS star-forming galaxies atz = 0.8–3.3
Publisher: Oxford University Press (OUP)
Date: 15-03-2019
DOI: 10.1093/MNRAS/STZ765
RED NUGGETS ATz∼ 1.5: COMPACT PASSIVE GALAXIES AND THE FORMATION OF THE KORMENDY RELATION
Publisher: American Astronomical Society
Date: 27-03-2009
Evidence for the spin-0 nature of the Higgs boson using ATLAS data
Publisher: Elsevier BV
Date: 10-2013
Ganaxolone versus Phenobarbital for Neonatal Seizure Management
Publisher: Wiley
Date: 26-09-2022
DOI: 10.1002/ANA.26493
Abstract: Seizures are more common in the neonatal period than at any other stage of life. Phenobarbital is the first‐line treatment for neonatal seizures and is at best effective in approximately 50% of babies, but may contribute to neuronal injury. Here, we assessed the efficacy of phenobarbital versus the synthetic neurosteroid, ganaxolone, to moderate seizure activity and neuropathology in neonatal lambs exposed to perinatal asphyxia. Asphyxia was induced via umbilical cord occlusion in term lambs at birth. Lambs were treated with ganaxolone (5mg/kg/bolus then 5mg/kg/day for 2 days) or phenobarbital (20mg/kg/bolus then 5mg/kg/day for 2 days) at 6 hours. Abnormal brain activity was classified as stereotypic evolving (SE) seizures, epileptiform discharges (EDs), and epileptiform transients (ETs) using continuous litude‐integrated electroencephalographic recordings. At 48 hours, lambs were euthanized for brain pathology. Asphyxia caused abnormal brain activity, including SE seizures that peaked at 18 to 20 hours, EDs, and ETs, and induced neuronal degeneration and neuroinflammation. Ganaxolone treatment was associated with an 86.4% reduction in the number of seizures compared to the asphyxia group. The total seizure duration in the asphyxia+ganaxolone group was less than the untreated asphyxia group. There was no difference in the number of SE seizures between the asphyxia and asphyxia+phenobarbital groups or duration of SE seizures. Ganaxolone treatment, but not phenobarbital, reduced neuronal degeneration within hippoc al CA1 and CA3 regions, and cortical neurons, and ganaxolone reduced neuroinflammation within the thalamus. Ganaxolone provided better seizure control than phenobarbital in this perinatal asphyxia model and was neuroprotective for the newborn brain, affording a new therapeutic opportunity for treatment of neonatal seizures. ANN NEUROL 2022 :1066–1079
The WiggleZ Dark Energy Survey: the transition to large-scale cosmic homogeneity
Publisher: Oxford University Press (OUP)
Date: 26-07-2012
The WiggleZ Dark Energy Survey: mapping the distance-redshift relation with baryon acoustic oscillations
Publisher: Oxford University Press (OUP)
Date: 04-10-2011
The Dawes Review 1: Kinematic Studies of Star-Forming Galaxies Across Cosmic Time
Publisher: Cambridge University Press (CUP)
Date: 2013
DOI: 10.1017/PASA.2013.34
Abstract: The last seven years have seen an explosion in the number of Integral Field galaxy surveys, obtaining resolved 2D spectroscopy, especially at high-redshift. These have taken advantage of the mature capabilities of 8–10 m class telescopes and the development of associated technology such as AO. Surveys have leveraged both high spectroscopic resolution enabling internal velocity measurements and high spatial resolution from AO techniques and sites with excellent natural seeing. For the first time, we have been able to glimpse the kinematic state of matter in young, assembling star-forming galaxies and learn detailed astrophysical information about the physical processes and compare their kinematic scaling relations with those in the local Universe. Observers have measured disc galaxy rotation, merger signatures, and turbulence-enhanced velocity dispersions of gas-rich discs. Theorists have interpreted kinematic signatures of galaxies in a variety of ways (rotation, merging, outflows, and feedback) and attempted to discuss evolution vs. theoretical models and relate it to the evolution in galaxy morphology. A key point that has emerged from this activity is that substantial fractions of high-redshift galaxies have regular kinematic morphologies despite irregular photometric morphologies and this is likely due to the presence of a large number of highly gas-rich discs. There has not yet been a review of this burgeoning topic. In this first Dawes review, I will discuss the extensive kinematic surveys that have been done and the physical models that have arisen for young galaxies at high-redshift.
Identification of Galaxy–Galaxy Strong Lens Candidates in the DECam Local Volume Exploration Survey Using Machine Learning
Publisher: American Astronomical Society
Date: 23-08-2023
Abstract: We perform a search for galaxy–galaxy strong lens systems using a convolutional neural network (CNN) applied to imaging data from the first public data release of the DECam Local Volume Exploration Survey, which contains ∼520 million astronomical sources covering ∼4000 deg 2 of the southern sky to a 5 σ point–source depth of g = 24.3, r = 23.9, i = 23.3, and z = 22.8 mag. Following the methodology of similar searches using Dark Energy Camera data, we apply color and magnitude cuts to select a catalog of ∼11 million extended astronomical sources. After scoring with our CNN, the highest-scoring 50,000 images were visually inspected and assigned a score on a scale from 0 (not a lens) to 3 (very probable lens). We present a list of 581 strong lens candidates, 562 of which are previously unreported. We categorize our candidates using their human-assigned scores, resulting in 55 Grade A candidates, 149 Grade B candidates, and 377 Grade C candidates. We additionally highlight eight potential quadruply lensed quasars from this s le. Due to the location of our search footprint in the northern Galactic cap ( b 10 deg) and southern celestial hemisphere (decl. 0 deg), our candidate list has little overlap with other existing ground-based searches. Where our search footprint does overlap with other searches, we find a significant number of high-quality candidates that were previously unidentified, indicating a degree of orthogonality in our methodology. We report properties of our candidates including apparent magnitude and Einstein radius estimated from the image separation.
A Compact Cluster of Massive Red Galaxies at a Redshift of 1.5
Publisher: American Astronomical Society
Date: 28-06-2007
DOI: 10.1086/520575
[ITAL]Hubble Space Telescope[/ITAL] Imaging of the CFRS and LDSS Redshift Surveys. III. Field Elliptical Galaxies at [FORMULA][F]0.2<z<1.0[/F][/FORMULA]
Publisher: American Astronomical Society
Date: 11-1999
DOI: 10.1086/307885
A Lyα-only Active Galactic Nucleus from the Sloan Digital Sky Survey
Publisher: American Astronomical Society
Date: 06-2004
DOI: 10.1086/420804
The Type Ia Supernova Rate at z ∼ 0.4
Publisher: American Astronomical Society
Date: 10-12-1996
DOI: 10.1086/178150
Early Results from GLASS-JWST. II. NIRCam Extragalactic Imaging and Photometric Catalog
Publisher: American Astronomical Society
Date: 10-2022
Abstract: We present the reduced images and multiwavelength catalog of the first JWST NIRCam extragalactic observations from the GLASS Early Release Science Program, obtained as coordinated parallels of the NIRISS observations of the Abell 2744 cluster. Images in seven bands (F090W, F115W, F150W, F200W, F277W, F356W, and F444W) have been reduced using an augmented version of the official JWST pipeline we discuss the procedures adopted to remove or mitigate defects in the raw images. We obtain a multiband catalog by means of forced aperture photometry on point-spread function (PSF)-matched images at the position of F444W-detected sources. The catalog is intended to enable early scientific investigations, and it is optimized for faint galaxies it contains 6368 sources, with limiting magnitude 29.7 at 5 σ in F444W. We release both images and catalog in order to allow the community to become familiar with the JWST NIRCam data and evaluate their merit and limitations given the current level of knowledge of the instrument.
Cosmological constraints from the SDSS luminous red galaxies
Publisher: American Physical Society (APS)
Date: 11-12-2006
The morphological identification of the rapidly evolving population of faint galaxies
Publisher: Oxford University Press (OUP)
Date: 07-1995
EXTREME GAS FRACTIONS IN CLUMPY, TURBULENT DISK GALAXIES AT z ∼ 0.1
Publisher: American Astronomical Society
Date: 18-07-2014
Corrigendum to “Measurements of Higgs boson production and couplings in diboson final states with the ATLAS detector at the LHC” [Phys. Lett. B 726 (1–3) (2013) 88]
Publisher: Elsevier BV
Date: 06-2014
ZFIRE
Publisher: American Astronomical Society
Date: 22-06-2016
First cosmology results using type Ia supernovae from the Dark Energy Survey: the effect of host galaxy properties on supernova luminosity
Publisher: Oxford University Press (OUP)
Date: 13-04-2020
Abstract: We present improved photometric measurements for the host galaxies of 206 spectroscopically confirmed type Ia supernovae discovered by the Dark Energy Survey Supernova Program (DES-SN) and used in the first DES-SN cosmological analysis. For the DES-SN s le, when considering a 5D (z, x1, c, α, β) bias correction, we find evidence of a Hubble residual ‘mass step’, where SNe Ia in high-mass galaxies (& M⊙) are intrinsically more luminous (after correction) than their low-mass counterparts by $\\gamma =0.040\\pm 0.019$ mag. This value is larger by 0.031 mag than the value found in the first DES-SN cosmological analysis. This difference is due to a combination of updated photometric measurements and improved star formation histories and is not from host-galaxy misidentification. When using a 1D (redshift-only) bias correction the inferred mass step is larger, with $\\gamma =0.066\\pm 0.020$ mag. The 1D−5D γ difference for DES-SN is $0.026\\pm 0.009$ mag. We show that this difference is due to a strong correlation between host galaxy stellar mass and the x1 component of the 5D distance-bias correction. Including an intrinsic correlation between the observed properties of SNe Ia, stretch and colour, and stellar mass in simulated SN Ia s les, we show that a 5D fit recovers γ with −9 mmag bias compared to a +2 mmag bias for a 1D fit. This difference can explain part of the discrepancy seen in the data. Improvements in modelling correlations between galaxy properties and SN is necessary to ensure unbiased precision estimates of the dark energy equation of state as we enter the era of LSST.
Angular momentum evolution of bulge stars in disc galaxies in NIHAO
Publisher: Oxford University Press (OUP)
Date: 10-11-2019
The influence of angular momentum and environment on the H i gas of late-type galaxies
Publisher: Oxford University Press (OUP)
Date: 17-06-2020
Abstract: We use high-resolution H i data from the Westerbork H i Survey of Spiral and Irregular Galaxies (WHISP) to study the H i and angular momentum properties of a s le of 114 late-type galaxies. We explore the specific baryonic angular momentum–baryonic mass (jb–Mb) relation, and find that an unbroken power law of the form $j_\\mathrm{ b} \\propto M_\\mathrm{ b}^{0.55 \\pm 0.02}$ fits the data well, with an intrinsic scatter of ∼0.13 ± 0.01 dex. We revisit the relation between the atomic gas fraction, fatm, and the integrated atomic stability parameter q (the fatm–q relation), originally introduced by Obreschkow et al., and probe this parameter space by populating it with galaxies from different environments, in order to study the influence of the environment on their jb, fatm, and q values. We find evidence that galaxies with close neighbours show a larger intrinsic scatter about the fatm–q relation compared to galaxies without close neighbours. We also find enhanced star formation rate among the deviating galaxies with close neighbours. In addition, we use the bulge-to-total (B/T) ratio as a morphology proxy, and find a general trend of decreasing B/T values with increasing disc stability and H i fraction in the fatm–q plane, indicating a fundamental link between mass, specific angular momentum, gas fraction, and morphology of galaxies.
Weak lensing of Type Ia Supernovae from the Dark Energy Survey
Publisher: Oxford University Press (OUP)
Date: 29-06-2020
Abstract: We consider the effects of weak gravitational lensing on observations of 196 spectroscopically confirmed Type Ia Supernovae (SNe Ia) from years 1 to 3 of the Dark Energy Survey (DES). We simultaneously measure both the angular correlation function and the non-Gaussian skewness caused by weak lensing. This approach has the advantage of being insensitive to the intrinsic dispersion of SNe Ia magnitudes. We model the litude of both effects as a function of σ8, and find σ8 =1.2$^{+0.9}_{-0.8}$. We also apply our method to a subs le of 488 SNe from the Joint Light-curve Analysis (JLA chosen to match the redshift range we use for this work), and find σ8 =0.8$^{+1.1}_{-0.7}$. The comparable uncertainty in σ8 between DES–SN and the larger number of SNe from JLA highlights the benefits of homogeneity of the DES–SN s le, and improvements in the calibration and data analysis.
The WiggleZ Dark Energy Survey: Direct constraints on blue galaxy intrinsic alignments at intermediate redshifts
Publisher: Oxford University Press (OUP)
Date: 05-10-2011
The stellar mass–size relation for cluster galaxies at z = 1 with high angular resolution from the Gemini/GeMS multiconjugate adaptive optics system
Publisher: Oxford University Press (OUP)
Date: 23-09-2016
zfourge: Extreme 5007 Å Emission May Be a Common Early-lifetime Phase for Star-forming Galaxies at z > 2.5
Publisher: American Astronomical Society
Date: 19-12-2018
Kinematic modelling of disc galaxies using graphics processing units
Publisher: Oxford University Press (OUP)
Date: 06-11-2015
The Effects of Environment on the Evolution of the Galaxy Stellar Mass Function
Publisher: American Astronomical Society
Date: 08-02-2018
FORTIS: pathfinder to the Lyman continuum
Publisher: SPIE
Date: 11-10-2004
DOI: 10.1117/12.552799
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions atz∼ 1.4
Publisher: Oxford University Press (OUP)
Date: 26-04-2016
DOI: 10.1093/PASJ/PSW029
The physical parameters of the evolving population of faint galaxies
Publisher: Oxford University Press (OUP)
Date: 07-1998
Low Star Formation Activity and Low Gas Content of Quiescent Galaxies at z = 3.5–4.0 Constrained with ALMA
Publisher: American Astronomical Society
Date: 31-08-2022
Abstract: The discovery in deep near-infrared surveys of a population of massive quiescent galaxies at z 3 has given rise to the question of how they came to be quenched so early in the history of the universe. Measuring their molecular gas properties can distinguish between physical processes where they stop forming stars due to a lack of fuel versus those where the star formation efficiency is reduced and the gas is retained. We conducted Atacama Large Millimeter/submillimeter Array observations of four quiescent galaxies at z = 3.5–4.0 found by the Fourstar Galaxy Evolution Survey and a serendipitous optically dark galaxy at z = 3.71. We aim to investigate the presence of dust-obscured star formation and their gas content by observing the dust continuum emission at Band 7 and the atomic carbon [C i ]( 3 P 1 – 3 P 0 ) line at 492.16 GHz. Among the four quiescent galaxies, only one source is detected in the dust continuum at λ obs = 870 μ m. The submillimeter observations confirm their passive nature, and all of them are located more than four times below the main sequence of star-forming galaxies at z = 3.7. None of the targets are detected in [C i ], constraining their gas-mass fractions to be %. These gas-mass fractions are more than 3 times lower than the scaling relation for star-forming galaxies at z = 3.7. These results support scenarios where massive galaxies at z = 3.5–4.0 quench by consuming/expelling all the gas rather than by reducing the efficiency of the conversion of their gas into stars.
The WiggleZ Dark Energy Survey: testing the cosmological model with baryon acoustic oscillations at z= 0.6
Publisher: Oxford University Press (OUP)
Date: 23-06-2011
Discovery of Extreme [O III]+Hβ Emitting Galaxies Tracing an Overdensity at z ̃ 3.5 in CDF-South
Publisher: American Astronomical Society
Date: 24-03-2017
First Cosmology Results using Supernovae Ia from the Dark Energy Survey: Survey Overview, Performance, and Supernova Spectroscopy
Publisher: American Astronomical Society
Date: 18-11-2020
Stellar angular momentum distribution linked to galaxy morphology
Publisher: Oxford University Press (OUP)
Date: 20-04-2020
Abstract: We study the spatially resolved stellar specific angular momentum j* in a high-quality s le of 24 Calar Alto Legacy Integral Field Area galaxies covering a broad range of visual morphology, accounting for stellar velocity and velocity dispersion. The shape of the spaxelwise probability density function of normalized s = j*/j*mean, PDF(s), deviates significantly from the near-universal initial distribution expected of baryons in a dark matter halo and can be explained by the expected baryonic effects in galaxy formation that remove and redistribute angular momentum. Further we find that the observed shape of the PDF(s) correlates significantly with photometric morphology, where late-type galaxies have a PDF(s) that is similar to a normal distribution, whereas early types have a strongly skewed PDF(s) resulting from an excess of low-angular momentum material. Galaxies that are known to host pseudo-bulges (bulge Sérsic index nb & 2.2) tend to have less skewed bulge PDF(s), with skewness (b1rb) ≲ 0.8. The PDF(s) encodes both kinematic and photometric information and appears to be a robust tracer of morphology. Its use is motivated by the desire to move away from traditional component-based classifications which are subject to observer bias, to classification on a galaxy’s fundamental (stellar mass and angular momentum) properties. In future, PDF(s) may also be useful as a kinematic decomposition tool.
Early Results from GLASS-JWST. VII. Evidence for Lensed, Gravitationally Bound Protoglobular Clusters at z = 4 in the Hubble Frontier Field A2744*
Publisher: American Astronomical Society
Date: 12-2022
Abstract: We investigate the blue and optical rest-frame sizes ( λ ≃ 2300–4000 Å) of three compact star-forming regions in a galaxy at z = 4 strongly lensed (×30, ×45, and ×100) by the Hubble Frontier Field galaxy cluster A2744 using GLASS-ERS James Webb Space Telescope (JWST)/NIRISS imaging at 1.15 μ m, 1.50 μ m, and 2.0 μ m with a point-spread function ≲0.″1. In particular, the Balmer break is probed in detail for all multiply imaged sources of the system. With ages of a few tens of Myr, stellar masses in the range (0.7–4.0) ×10 6 M ⊙ and optical/ultraviolet effective radii spanning the interval 3 R eff 20 pc, such objects are currently the highest-redshift (spectroscopically confirmed) gravitationally bound young massive star clusters (YMCs), with stellar mass surface densities resembling those of local globular clusters. Optical (4000 Å, JWST-based) and ultraviolet (1600 Å, Hubble Space Telescope–based) sizes are fully compatible. The contribution to the ultraviolet underlying continuum emission (1600 Å) is ∼30%, which decreases by a factor of 2 in the optical for two of the YMCs (∼4000 Å rest-frame), reflecting the young ages ( Myr) inferred from the spectral energy distribution fitting and supported by the presence of high-ionization lines secured with the Very Large Telescope/MUSE. Such bursty forming regions enhance the specific star formation rate of the galaxy, which is ≃10 Gyr −1 . This galaxy would be among the extreme analogs observed in the local universe having a high star formation rate surface density and a high occurrence of massive stellar clusters in formation.
The WiggleZ Dark Energy Survey: constraining galaxy bias and cosmic growth with three-point correlation functions
Publisher: Oxford University Press (OUP)
Date: 24-05-2013
DOI: 10.1093/MNRAS/STT520
Early Results from GLASS-JWST. I: Confirmation of Lensed z ≥ 7 Lyman-break Galaxies behind the Abell 2744 Cluster with NIRISS
Publisher: American Astronomical Society
Date: 10-2022
Abstract: We present the first search for z ≥ 7, continuum-confirmed Lyman break sources with NIRISS/WFS spectroscopy over the Abell 2744 Frontier Fields cluster, as part of the GLASS-JWST-ERS survey. With ∼15 hr of preimaging and multiangle grism exposures in the F115W, F150W, and F200W filters, we describe the general data handling (i.e., reduction, cleaning, modeling, and extraction processes) and analysis for the GLASS-JWST survey. We showcase the power of JWST to peer deep into reionization, when most intergalactic hydrogen is neutral, by confirming two galaxies at z = 8.04 ± 0.15 and z = 7.90 ± 0.13 by means of their Lyman breaks. Fainter continuum spectra are observed in both the F150W and F200W bands, indicative of blue (−1.69 and −1.33) UV slopes and moderately bright absolute magnitudes (−20.37 and −19.68 mag). We do not detect strong Ly α in either galaxy, but do observe tentative (∼2.7–3.8 σ ) He ii λ 1640 Å, O iii ] λλ 1661,1666 Å, and N iii ] λλ 1747,1749 Å line emission in one, suggestive of low-metallicity, star-forming systems with possible nonthermal contributions. These novel observations provide a first look at the extraordinary potential of JWST/NIRISS for confirming representative s les of bright z ≥ 7 sources in the absence of strong emission lines, and gain unprecedented insight into their contributions toward cosmic reionization.
The WiggleZ Dark Energy Survey: probing the epoch of radiation domination using large-scale structure
Publisher: Oxford University Press (OUP)
Date: 04-01-2013
DOI: 10.1093/MNRAS/STS431
Optimizing baryon acoustic oscillation surveys - I. Testing the concordance CDM cosmology
Publisher: Oxford University Press (OUP)
Date: 05-2007
ZFOURGE: Using Composite Spectral Energy Distributions to Characterize Galaxy Populations at 1 < z < 4
Publisher: American Astronomical Society
Date: 17-08-2018
The AGEL Survey: Spectroscopic Confirmation of Strong Gravitational Lenses in the DES and DECaLS Fields Selected Using Convolutional Neural Networks
Publisher: American Astronomical Society
Date: 26-09-2022
Abstract: We present spectroscopic confirmation of candidate strong gravitational lenses using the Keck Observatory and Very Large Telescope as part of our ASTRO 3D Galaxy Evolution with Lenses ( AGEL ) survey. We confirm that (1) search methods using convolutional neural networks (CNNs) with visual inspection successfully identify strong gravitational lenses and (2) the lenses are at higher redshifts relative to existing surveys due to the combination of deeper and higher-resolution imaging from DECam and spectroscopy spanning optical to near-infrared wavelengths. We measure 104 redshifts in 77 systems selected from a catalog in the DES and DECaLS imaging fields ( r ≤ 22 mag). Combining our results with published redshifts, we present redshifts for 68 lenses and establish that CNN-based searches are highly effective for use in future imaging surveys with a success rate of at least 88% (defined as 68/77). We report 53 strong lenses with spectroscopic redshifts for both the deflector and source ( z src z defl ), and 15 lenses with a spectroscopic redshift for either the deflector ( z defl 0.21) or source ( z src ≥ 1.34). For the 68 lenses, the deflectors and sources have average redshifts and standard deviations of 0.58 ± 0.14 and 1.92 ± 0.59 respectively, and corresponding redshift ranges of z defl = 0.21–0.89 and z src = 0.88–3.55. The AGEL systems include 41 deflectors at z defl ≥ 0.5 that are ideal for follow-up studies to track how mass density profiles evolve with redshift. Our goal with AGEL is to spectroscopically confirm ∼100 strong gravitational lenses that can be observed from both hemispheres throughout the year. The AGEL survey is a resource for refining automated all-sky searches and addressing a range of questions in astrophysics and cosmology.
First Data Release of the COSMOS Ly α Mapping and Tomography Observations: 3D Ly α Forest Tomography at 2.
Publisher: American Astronomical Society
Date: 02-08-2018
Angular momentum of z ∼ 1.5 galaxies and their local analogues with adaptive optics
Publisher: Oxford University Press (OUP)
Date: 14-03-2019
DOI: 10.1093/MNRAS/STZ750
DYNAMO - II. Coupled stellar and ionized-gas kinematics in two low-redshift clumpy discs
Publisher: Oxford University Press (OUP)
Date: 30-06-2014
Effect of local environment and stellar mass on galaxy quenching and morphology at 0.5 < z < 2.0
Publisher: American Astronomical Society
Date: 03-10-2017
OBSERVATIONS OF THE NAKED-EYE GRB 080319B: IMPLICATIONS OF NATURE'S BRIGHTEST EXPLOSION
Publisher: American Astronomical Society
Date: 19-01-2009
Candidate Periodically Variable Quasars from the Dark Energy Survey and the Sloan Digital Sky Survey
Publisher: Oxford University Press (OUP)
Date: 26-09-2020
Abstract: Periodically variable quasars have been suggested as close binary supermassive black holes. We present a systematic search for periodic light curves in 625 spectroscopically confirmed quasars with a median redshift of 1.8 in a 4.6 deg2 overlapping region of the Dark Energy Survey Supernova (DES-SN) fields and the Sloan Digital Sky Survey Stripe 82 (SDSS-S82). Our s le has a unique 20-year long multi-color (griz) light curve enabled by combining DES-SN Y6 observations with archival SDSS-S82 data. The deep imaging allows us to search for periodic light curves in less luminous quasars (down to r ∼23.5 mag) powered by less massive black holes (with masses ≳ 108.5M⊙) at high redshift for the first time. We find five candidates with significant (at & .74% single-frequency significance in at least two bands with a global p-value of ∼7 × 10−4–3× 10−3 accounting for the look-elsewhere effect) periodicity with observed periods of ∼3–5 years (i.e., 1–2 years in rest frame) having ∼4–6 cycles spanned by the observations. If all five candidates are periodically variable quasars, this translates into a detection rate of ${\\sim }0.8^{+0.5}_{-0.3}$% or ${\\sim }1.1^{+0.7}_{-0.5}$ quasar per deg2. Our detection rate is 4–80 times larger than those found by previous searches using shallower surveys over larger areas. This discrepancy is likely caused by differences in the quasar populations probed and the survey data qualities. We discuss implications on the future direct detection of low-frequency gravitational waves. Continued photometric monitoring will further assess the robustness and characteristics of these candidate periodic quasars to determine their physical origins.
Decoupled black hole accretion and quenching: the relationship between BHAR, SFR and quenching in Milky Way- and Andromeda-mass progenitors since z = 2.5
Publisher: Oxford University Press (OUP)
Date: 09-10-2018
An Hα survey of the rich cluster A 1689
Publisher: Oxford University Press (OUP)
Date: 09-2002
Dark Energy Survey Year 3 results: A 2.7% measurement of baryon acoustic oscillation distance scale at redshift 0.835
Publisher: American Physical Society (APS)
Date: 08-02-2022
GRB 080503: IMPLICATIONS OF A NAKED SHORT GAMMA-RAY BURST DOMINATED BY EXTENDED EMISSION
Publisher: American Astronomical Society
Date: 27-04-2009
Finding strong lenses in CFHTLS using convolutional neural networks
Publisher: Oxford University Press (OUP)
Date: 15-06-2017
A population of faint, old, and massive quiescent galaxies at 3 < z < 4 revealed by JWST NIRSpec Spectroscopy
Publisher: Research Square Platform LLC
Date: 09-01-2023
DOI: 10.21203/RS.3.RS-2404918/V1
Abstract: The confirmation of the presence of very massive quiescent galaxies at epochs only 1–2 Gyr after the Big Bang [1–8] has challenged models of cosmology and galaxy formation [9]. Producing sufficient numbers of these requires abundant numbers of the host dark matter halos to have been assembled and sufficient time for star formation to proceed extremely quickly and then cease just as rapidly. Ground-based spectroscopy has suggested ages of 200–300 Myr[3] at redshifts 3 z 4. The true number and ages of these objects have however been highly uncertain as ground-based spectra has been limited to the bright- est of them [e.g. 3, 5], at wavelengths ∼ 2μm, which introduces a signficant potential bias towards younger objects [7]. The launch of the James Webb Space Telescope (JWST) enables dramatically more sensitive and constraining spectroscopic observations due to the very low sky background, sharp image quality, and access to wavelengths beyond 2μm. Here we report JWST NIR- Spec [10] (0.6–5.3μm) observations of five new quiescent galaxy candidates that were beyond the limit of previous ground-based spectroscopy. The high signal:noise spectra of galaxies with continuum significantly fainter than ear- lier confirmations show that they are also at redshifts 3 z 4, and that they have substantial stellar masses of ∼ 0.5−1.2×1011 M⊙ comparable to massive galaxies in the nearby Universe. One of the galaxies has been quenched for ∼ 1 billion years pointing to a presence of substantially older and fainter galaxies than those revealed so far by ground-based spectroscopy. This suggests that some of the massive galaxies have very early formation epochs (during the epoch of reionization, z ∼ 6) pointing to a need for high conversion rates of baryons to stars in the first massive galaxy halos in the early Universe [11, 12].
The Third Data Release of the Sloan Digital Sky Survey
Publisher: American Astronomical Society
Date: 03-2005
DOI: 10.1086/427544
ZFIRE: 3D Modeling of Rotation, Dispersion, and Angular Momentum of Star-forming Galaxies at z ∼ 2
Publisher: American Astronomical Society
Date: 03-05-2018
The Subaru FMOS Galaxy Redshift Survey (FastSound). III. The mass–metallicity relation and the fundamental metallicity relation atz ∼ 1.4
Publisher: Oxford University Press (OUP)
Date: 23-09-2015
DOI: 10.1093/PASJ/PSV079
The role of design issues in work-related fatal injury in Australia
Publisher: Elsevier BV
Date: 2008
DOI: 10.1016/J.JSR.2008.02.024
Abstract: This study aimed to provide an assessment of the contribution of design to the occurrence of fatal work-related injuries in Australia. The Australian National Coroners' Information System was the data source for fatal injuries. Deaths resulting from workplace injuries on or between 1 July 2000 and 30 June 2002 were included. Seventy seven (37%) of the 210 identified workplace fatalities definitely or probably had design-related issues involved. In another 29 (14%), the circumstances were suggestive that design issues were involved. The most common scenarios involved problems with rollover protective structures and/or associated seat belts inadequate guarding lack of residual current devices inadequate fall protection failed hydraulic lifting systems in vehicles and mobile equipment and inadequate protection mechanisms on mobile plant and vehicles. Design is a significant contributor to work-related fatal injury in Australia. There is considerable scope for preventing serious work-related injury through improving design of plant, equipment, and vehicles used for work-related purposes.
First results from Z-FOURGE
Publisher: American Astronomical Society
Date: 12-03-2012
Photometric redshifts for the Kilo-Degree Survey
Publisher: EDP Sciences
Date: 08-2018
DOI: 10.1051/0004-6361/201731942
Abstract: We present a machine-learning photometric redshift (ML photo- z ) analysis of the Kilo-Degree Survey Data Release 3 (KiDS DR3), using two neural-network based techniques: ANNz2 and MLPQNA. Despite limited coverage of spectroscopic training sets, these ML codes provide photo- z s of quality comparable to, if not better than, those from the Bayesian Photometric Redshift (BPZ) code, at least up to z phot ≲ 0.9 and r ≲ 23.5. At the bright end of r ≲ 20, where very complete spectroscopic data overlapping with KiDS are available, the performance of the ML photo- z s clearly surpasses that of BPZ, currently the primary photo- z method for KiDS. Using the Galaxy And Mass Assembly (GAMA) spectroscopic survey as calibration, we furthermore study how photo- z s improve for bright sources when photometric parameters additional to magnitudes are included in the photo- z derivation, as well as when VIKING and WISE infrared (IR) bands are added. While the fiducial four-band ugri setup gives a photo- z bias 〈 δz /(1 + z )〉 = −2 × 10 −4 and scatter σ δz/(1+z) 0.022 at mean 〈 z 〉 = 0.23, combining magnitudes, colours, and galaxy sizes reduces the scatter by ~7% and the bias by an order of magnitude. Once the ugri and IR magnitudes are joined into 12-band photometry spanning up to 12 μ m, the scatter decreases by more than 10% over the fiducial case. Finally, using the 12 bands together with optical colours and linear sizes gives 〈 δz /(1 + z )〉 4 × 10 −5 and σ δz /(1+ z ) 0.019. This paper also serves as a reference for two public photo- z catalogues accompanying KiDS DR3, both obtained using the ANNz2 code. The first one, of general purpose, includes all the 39 million KiDS sources with four-band ugri measurements in DR3. The second dataset, optimised for low-redshift studies such as galaxy-galaxy lensing, is limited to r ≲ 20, and provides photo- z s of much better quality than in the full-depth case thanks to incorporating optical magnitudes, colours, and sizes in the GAMA-calibrated photo- z derivation.
Early Results from GLASS-JWST. XIII. A Faint, Distant, and Cold Brown Dwarf*
Publisher: American Astronomical Society
Date: 2023
Abstract: We present the serendipitous discovery of a late T-type brown dwarf candidate in JWST NIRCam observations of the Early Release Science Abell 2744 parallel field. The discovery was enabled by the sensitivity of JWST at 4 μ m wavelengths and the panchromatic 0.9–4.5 μ m coverage of the spectral energy distribution. The unresolved point source has magnitudes F115W = 27.95 ± 0.15 and F444W = 25.84 ± 0.01 (AB), and its F115W−F444W and F356W−F444W colors match those expected for other known T dwarfs. We can exclude it as a reddened background star, high redshift quasar, or a very high redshift galaxy. Comparison with stellar atmospheric models indicates a temperature of T eff ≈ 650 K and surface gravity log g ≈ 5.25 , implying a mass of 0.03 M ⊙ and age of 5 Gyr. We estimate the distance of this candidate to be 570–720 pc in a direction perpendicular to the Galactic plane, making it a likely thick disk or halo brown dwarf. These observations underscore the power of JWST to probe the very low-mass end of the substellar mass function in the Galactic thick disk and halo.
The Subaru FMOS galaxy redshift survey (FastSound). II. The emission line catalog and properties of emission line galaxies
Publisher: Oxford University Press (OUP)
Date: 25-05-2016
DOI: 10.1093/PASJ/PSW043
DUVET: Spatially Resolved Observations of Star Formation Regulation via Galactic Outflows in a Starbursting Disk Galaxy
Publisher: American Astronomical Society
Date: 12-2022
Abstract: We compare 500 pc scale, resolved observations of ionized and molecular gas for the z ∼ 0.02 starbursting disk galaxy IRAS08339+6517, using measurements from KCWI and NOEMA. We explore the relationship of the star-formation-driven ionized gas outflows with colocated galaxy properties. We find a roughly linear relationship between the outflow mass flux ( Σ ̇ out ) and star formation rate surface density (Σ SFR ), Σ ̇ out ∝ Σ SFR 1.06 ± 0.10 , and a strong correlation between Σ ̇ out and the gas depletion time, such that Σ ̇ out ∝ t dep − 1.1 ± 0.06 . Moreover, we find these outflows are so-called breakout outflows, according to the relationship between the gas fraction and disk kinematics. Assuming that ionized outflow mass scales with total outflow mass, our observations suggest that the regions of highest Σ SFR in IRAS08 are removing more gas via the outflow than through the conversion of gas into stars. Our results are consistent with a picture in which the outflow limits the ability of a region of a disk to maintain short depletion times. Our results underline the need for resolved observations of outflows in more galaxies.
Anglo-Australian Observatory 2dF project: a status report after the first year of scientific operation
Publisher: SPIE
Date: 09-07-1998
DOI: 10.1117/12.316796
Faint galaxies: evolution and cosmological curvature
Publisher: Springer Science and Business Media LLC
Date: 1992
DOI: 10.1038/355055A0
Differences in the Structural Properties and Star-formation Rates of Field and Cluster Galaxies at z~1
Publisher: American Astronomical Society
Date: 21-07-2016
THE SAMI GALAXY SURVEY: TOWARD A UNIFIED DYNAMICAL SCALING RELATION FOR GALAXIES OF ALL TYPES
Publisher: American Astronomical Society
Date: 29-10-2014
The GLASS-JWST Early Release Science Program. II. Stage I Release of NIRCam Imaging and Catalogs in the Abell 2744 Region
Publisher: American Astronomical Society
Date: 07-2023
Abstract: We present images and a multiwavelength photometric catalog based on all of the JWST NIRCam observations obtained to date in the region of the Abell 2744 galaxy cluster. These data come from three different programs, namely, the GLASS-JWST Early Release Science Program, UNCOVER, and the Director’s Discretionary Time program 2756. The observed area in the NIRCam wide-band filters—covering the central and extended regions of the cluster, as well as new parallel fields—is 46.5 arcmin 2 in total. All images in eight bands (F090W, F115W, F150W, F200W, F277W, F356W, F410M, and F444W) have been reduced adopting the latest calibration and reference files available. Data reduction has been performed using an augmented version of the official JWST pipeline, with improvements aimed at removing or mitigating defects in the raw images and improving the background subtraction and photometric accuracy. We obtain an F444W-detected multiband catalog, including all NIRCam and available Hubble Space Telescope data, adopting forced-aperture photometry on point-spread-function-matched images. The catalog is intended to enable early scientific investigations and is optimized for the study of faint galaxies it contains 24,389 sources, with a 5 σ limiting magnitude in the F444W band ranging from 28.5 AB to 30.5 AB, as a result of the varying exposure times of the surveys that observed the field. We publicly release the reduced NIRCam images, associated multiwavelength catalog, and the code adopted for 1/ f noise removal with the aim of aiding users in familiarizing themselves with JWST NIRCam data and identifying suitable targets for follow-up observations.
Gas Content and Kinematics in Clumpy, Turbulent Star-forming Disks
Publisher: American Astronomical Society
Date: 29-08-2017
Massive high-redshift quiescent galaxies with JWST
Publisher: Cambridge University Press (CUP)
Date: 2022
DOI: 10.1017/PASA.2021.61
Abstract: Recent ground-based deep observations of the Universe have discovered large populations of massive quiescent galaxies at $z\\sim3\\!-\\!5$ . With the launch of the James Webb Space Telescope (JWST) , the on-board Near-Infrared Spectrograph (NIRSpec) instrument will provide continuous $0.6\\!-\\!5.3\\,\\unicode{x03BC}\\,\\mathrm{m}$ spectroscopic coverage of these galaxies. Here we show that NIRSpec/CLEAR spectroscopy is ideal to probe the completeness of photometrically selected massive quiescent galaxies such as the ones presented by Schreiber et al. (2018b, A& A, 618, A85). Using a subset of the Schreiber et al. (2018b, A& A, 618, A85) s le with deep Keck/MOSFIRE spectroscopy presented by Esdaile J., et al. (2021b, ApJ, 908, L35), we perform a suite of mock JWST/NIRSpec observations to determine optimal observing strategies to efficiently recover the star formation histories (SFHs), element abundances, and kinematics of these massive quiescent galaxies. We find that at $z\\sim3$ , medium resolution G235M/FL170LP NIRSpec observations could recover element abundances at an accuracy of ${\\sim}15\\%$ , which is comparable to local globular clusters. Mimicking ZFOURGE COSMOS photometry, we perform mock spectrophotometric fitting with Prospector to show that the overall shape of the SFHs of our mock galaxies can be recovered well, albeit with a dependency on the number of non-parametric SFH bins. We show that deep high-resolution G235H/FL170LP integral field spectroscopy with a $S/N\\sim7$ per spaxel is required to constrain the rotational properties of our s le at $ \\!2\\sigma$ confidence. Thus, through optimal grism/filter choices, JWST/NIRSpec slit and integral field spectroscopy observations would provide tight constraints to galaxy evolution in the early Universe.
OzDES multifibre spectroscopy for the Dark Energy Survey: first-year operation and results
Publisher: Oxford University Press (OUP)
Date: 29-07-2015
The Gemini Deep Deep Survey. II. Metals in Star‐forming Galaxies at Redshift 1.3 < z < 2
Publisher: American Astronomical Society
Date: 10-02-2004
DOI: 10.1086/380903
First Cosmology Results Using SNe Ia from the Dark Energy Survey: Analysis, Systematic Uncertainties, and Validation
Publisher: American Astronomical Society
Date: 02-04-2019
The Science Case for PILOT I: Summary and Overview
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08048
Abstract: PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. Conditions at Dome C are known to be exceptional for astronomy. The seeing (above ∼30 m height), coherence time, and isoplanatic angle are all twice as good as at typical mid-latitude sites, while the water-vapour column, and the atmosphere and telescope thermal emission are all an order of magnitude better. These conditions enable a unique scientific capability for PILOT, which is addressed in this series of papers. The current paper presents an overview of the optical and instrumentation suite for PILOT and its expected performance, a summary of the key science goals and observational approach for the facility, a discussion of the synergies between the science goals for PILOT and other telescopes, and a discussion of the future of Antarctic astronomy. Paper II and Paper III present details of the science projects ided, respectively, between the distant Universe (i.e. studies of first light, and the assembly and evolution of structure) and the nearby Universe (i.e. studies of Local Group galaxies, the Milky Way, and the Solar System).
The Science Case for PILOT II: the Distant Universe
Publisher: Cambridge University Press (CUP)
Date: 2009
DOI: 10.1071/AS08049
Abstract: PILOT (the Pathfinder for an International Large Optical Telescope) is a proposed 2.5-m optical/infrared telescope to be located at Dome C on the Antarctic plateau. The atmospheric conditions at Dome C deliver a high sensitivity, high photometric precision, wide-field, high spatial resolution, and high-cadence imaging capability to the PILOT telescope. These capabilities enable a unique scientific potential for PILOT, which is addressed in this series of papers. The current paper presents a series of projects dealing with the distant (redshift ) Universe, that have been identified as key science drivers for the PILOT facility. The potential for PILOT to detect the first populations of stars to form in the early Universe, via infrared projects searching for pair-instability supernovae and gamma-ray burst afterglows, is investigated. Two projects are proposed to examine the assembly and evolution of structure in the Universe: an infrared survey searching for the first evolved galaxies at high redshift, and an optical survey aimed at characterising moderate-redshift galaxy clusters. Finally, a large-area weak-lensing survey and a program to obtain supernova infrared light-curves are proposed to examine the nature and evolution of dark energy and dark matter.
First Cosmology Results using Type Ia Supernovae from the Dark Energy Survey: Constraints on Cosmological Parameters
Publisher: American Astronomical Society
Date: 21-02-2019
Revisiting the Stellar Mass-Angular Momentum-Morphology Relation
Publisher: American Astronomical Society
Date: 08-05-0006
The WiggleZ Dark Energy Survey: measuring the cosmic expansion history using the Alcock-Paczynski test and distant supernovae
Publisher: Oxford University Press (OUP)
Date: 04-10-2011
Exploring the interpretability of deep neural networks used for gravitational lens finding with a sensitivity probe
Publisher: Elsevier BV
Date: 2022
Size Scaling of Clump Instabilities in Turbulent, Feedback-regulated Disks
Publisher: American Astronomical Society
Date: 04-04-2019
Satellite Quenching and Galactic Conformity at 0.3 〈 z 〈 2.5
Publisher: American Astronomical Society
Date: 19-01-2016
Autofib Redshift Survey - I. Evolution of the galaxy luminosity function
Publisher: Oxford University Press (OUP)
Date: 05-1996
Observation of a new particle in the search for the Standard Model Higgs boson with the ATLAS detector at the LHC
Publisher: Elsevier BV
Date: 09-2012
Present and Future of Surface-Enhanced Raman Scattering
Publisher: American Chemical Society (ACS)
Date: 03-09-2019
Closing in on the sources of cosmic reionization: First results from the GLASS-JWST program
Publisher: EDP Sciences
Date: 04-2023
DOI: 10.1051/0004-6361/202345866
Abstract: The escape fraction of Lyman-continuum (LyC) photons ( f esc ) is a key parameter for determining the sources of cosmic reionization at z ≥ 6. At these redshifts, owing to the opacity of the intergalactic medium, the LyC emission cannot be measured directly. However, LyC leakers during the epoch of reionization could be identified using indirect indicators that have been extensively tested at low and intermediate redshifts. These include a high [O III ]/[O II ] flux ratio, high star-formation surface density, and compact sizes. In this work, we present observations of 29 4.5 ≤ z ≤ 8 gravitationally lensed galaxies in the Abell 2744 cluster field. From a combined analysis of JWST-NIRSpec and NIRCam data, we accurately derived their physical and spectroscopic properties: our galaxies have low masses (log( M ⋆ )∼8.5), blue UV spectral slopes ( β ∼ −2.1), compact sizes ( r e ∼ 0.3 − 0.5 kpc), and high [O III ]/[O II ] flux ratios. We confirm that these properties are similar to those characterizing low-redshift LyC leakers. Indirectly inferring the fraction of escaping ionizing photons, we find that more than 80% of our galaxies have predicted f esc values larger than 0.05, indicating that they would be considered leakers. The average predicted f esc value of our s le is 0.12, suggesting that similar galaxies at z ≥ 6 have provided a substantial contribution to cosmic reionization.
An Efficient Approach to Obtaining Large Numbers of Distant Supernova Host Galaxy Redshifts
Publisher: Cambridge University Press (CUP)
Date: 2013
Abstract: We use the wide-field capabilities of the 2 degree field fibre positioner and the AAOmega spectrograph on the Anglo-Australian Telescope (AAT) to obtain redshifts of galaxies that hosted supernovae during the first 3 years of the Supernova Legacy Survey (SNLS). With exposure times ranging from 10 to 60 ks per galaxy, we were able to obtain redshifts for 400 host galaxies in two SNLS fields, thereby substantially increasing the total number of SNLS supernovae with host galaxy redshifts. The median redshift of the galaxies in our s le that hosted photometrically classified Type Ia supernovae (SNe Ia) is z ~ 0.77, which is 25% higher than the median redshift of spectroscopically confirmed SNe Ia in the 3-year s le of the SNLS. Our results demonstrate that one can use wide-field fibre-fed multi-object spectrographs on 4-m telescopes to efficiently obtain redshifts for large numbers of supernova host galaxies over the large areas of the sky that will be covered by future high-redshift supernova surveys, such as the Dark Energy Survey.
Testing Potential New Sites for Optical Telescopes in Australia
Publisher: Cambridge University Press (CUP)
Date: 2013
Abstract: In coming years, Australia may find the need to build new optical telescopes to continue local programmes, contribute to global survey projects, and form a local multi-wavelength connection for the new radio telescopes being built. In this study, we refine possible locations for a new optical telescope by studying remotely sensed meteorological infrared data to ascertain expected cloud coverage rates across Australia, and combine these data with a digital elevation model using a geographic information system. We find that the best sites within Australia for building optical telescopes are likely to be on the highest mountains in the Hamersley Range in northwest Western Australia, while the MacDonnell Ranges in the Northern Territory may also be appropriate. We believe that similar seeing values to Siding Spring should be obtainable and with significantly more observing time at the identified sites. We expect to find twice as many clear nights as at current telescope sites. These sites are thus prime locations for future on-site testing.
Studying Type II supernovae as cosmological standard candles using the Dark Energy Survey
Publisher: Oxford University Press (OUP)
Date: 22-05-2020
Abstract: Despite vast improvements in the measurement of the cosmological parameters, the nature of dark energy and an accurate value of the Hubble constant (H0) in the Hubble–Lemaître law remain unknown. To break the current impasse, it is necessary to develop as many independent techniques as possible, such as the use of Type II supernovae (SNe II). The goal of this paper is to demonstrate the utility of SNe II for deriving accurate extragalactic distances, which will be an asset for the next generation of telescopes where more-distant SNe II will be discovered. More specifically, we present a s le from the Dark Energy Survey Supernova Program (DES-SN) consisting of 15 SNe II with photometric and spectroscopic information spanning a redshift range up to 0.35. Combining our DES SNe with publicly available s les, and using the standard candle method (SCM), we construct the largest available Hubble diagram with SNe II in the Hubble flow (70 SNe II) and find an observed dispersion of 0.27 mag. We demonstrate that adding a colour term to the SN II standardization does not reduce the scatter in the Hubble diagram. Although SNe II are viable as distance indicators, this work points out important issues for improving their utility as independent extragalactic beacons: find new correlations, define a more standard subclass of SNe II, construct new SN II templates, and dedicate more observing time to high-redshift SNe II. Finally, for the first time, we perform simulations to estimate the redshift-dependent distance-modulus bias due to selection effects.
Extragalactic Fields Optimized for Adaptive Optics
Publisher: IOP Publishing
Date: 03-2011
DOI: 10.1086/658931
A test of SDSS aperture corrections using integral-field spectroscopy
Publisher: Oxford University Press (OUP)
Date: 15-05-2017
An Extended Catalog of Galaxy–Galaxy Strong Gravitational Lenses Discovered in DES Using Convolutional Neural Networks
Publisher: American Astronomical Society
Date: 19-07-2019
Probing Dark Energy Using Baryonic Oscillations in the Galaxy Power Spectrum as a Cosmological Ruler
Publisher: American Astronomical Society
Date: 10-09-2003
DOI: 10.1086/376983
Large molecular gas reservoirs in ancestors of Milky Way-mass galaxies nine billion years ago
Publisher: Springer Science and Business Media LLC
Date: 19-12-2016
Discovery of the Optical Counterpart and Early Optical Observations of GRB 990712
Publisher: American Astronomical Society
Date: 09-2000
DOI: 10.1086/309340
Constraints on a Universal Stellar Initial Mass Function from Ultraviolet to Near-Infrared Galaxy Luminosity Densities
Publisher: American Astronomical Society
Date: 10-08-2003
DOI: 10.1086/376502
Hubble Space Telescope Medium Deep Survey. II. Deconvolution of Wide Field Camera Field Galaxy Images in the 13h+43degree Field
Publisher: American Astronomical Society
Date: 03-1994
DOI: 10.1086/116907
A Glimpse of the Stellar Populations and Elemental Abundances of Gravitationally Lensed, Quiescent Galaxies at z ≳ 1 with Keck Deep Spectroscopy
Publisher: American Astronomical Society
Date: 05-2023
Abstract: Gravitational lenses can magnify distant galaxies, allowing us to discover and characterize the stellar populations of intrinsically faint, quiescent galaxies that are otherwise extremely difficult to directly observe at high redshift from ground-based telescopes. Here, we present the spectral analysis of two lensed, quiescent galaxies at z ≳ 1 discovered by the ASTRO 3D Galaxy Evolution with Lenses survey: AGEL 1323 ( M * ∼ 10 11.1 M ⊙ , z = 1.016, μ ∼ 14.6) and AGEL 0014 ( M * ∼ 10 11.5 M ⊙ , z = 1.374, μ ∼ 4.3). We measured the age, [Fe/H], and [Mg/Fe] of the two lensed galaxies using deep, rest-frame-optical spectra (S/N ≳40 Å −1 ) obtained on the Keck I telescope. The ages of AGEL 1323 and AGEL 0014 are 5.6 − 0.8 + 0.8 Gyr and 3.1 − 0.3 + 0.8 Gyr, respectively, indicating that most of the stars in the galaxies were formed less than 2 Gyr after the Big Bang. Compared to nearby quiescent galaxies of similar masses, the lensed galaxies have lower [Fe/H] and [Mg/H]. Surprisingly, the two galaxies have comparable [Mg/Fe] to similar-mass galaxies at lower redshifts, despite their old ages. Using a simple analytic chemical evolution model connecting the instantaneously recycled element Mg with the mass-loading factors of outflows averaged over the entire star formation history, we found that the lensed galaxies may have experienced enhanced outflows during their star formation compared to lower-redshift galaxies, which may explain why they quenched early.
Early Results from GLASS-JWST. IX. First Spectroscopic Confirmation of Low-mass Quiescent Galaxies at z > 2 with NIRISS
Publisher: American Astronomical Society
Date: 2023
Abstract: How passive galaxies form, and the physical mechanisms which prevent star formation over long timescales, are some of the most outstanding questions in understanding galaxy evolution. The properties of quiescent galaxies over cosmic time provide crucial information to identify the quenching mechanisms. Passive galaxies have been confirmed and studied out to z ∼ 4, but all of these studies have been limited to massive systems (mostly with log ( M star / M ⊙ ) 10.8 ). Using JWST-NIRISS grism slitless spectroscopic data from the GLASS-JWST Early Release Science program, we present spectroscopic confirmation of two quiescent galaxies at z spec = 2.650 − 0.006 + 0.004 and z spec = 2.433 − 0.016 + 0.032 (3 σ errors) with stellar masses of log ( M star / M ⊙ ) = 10.59 − 0.05 + 0.11 and log ( M star / M ⊙ ) = 10.07 − 0.03 + 0.06 (corrected for magnification factors of μ = 2.0 and μ = 2.1, respectively). The latter represents the first spectroscopic confirmation of the existence of low-mass quiescent galaxies at cosmic noon, showcasing the power of JWST to identify and characterize this enigmatic population.
A new candidate brown dwarf from an infrared survey.
Publisher: Oxford University Press (OUP)
Date: 09-1994
Z-FIRE
Publisher: American Astronomical Society
Date: 03-03-2016
THE GALAXY POPULATION HOSTING GAMMA-RAY BURSTS
Publisher: American Astronomical Society
Date: 09-01-2009
The nature of an ultra-faint galaxy in the cosmic dark ages seen with JWST
Publisher: Springer Science and Business Media LLC
Date: 17-05-2023
The WiggleZ Dark Energy Survey: star formation in UV-luminous galaxies from their luminosity functions
Publisher: Oxford University Press (OUP)
Date: 09-07-2013
Testing Feedback-regulated Star Formation in Gas-rich, Turbulent Disk Galaxies
Publisher: American Astronomical Society
Date: 04-01-2019
Discovery of Lyman Break Galaxies at z ~ 7 from the zFourGE Survey
Publisher: American Astronomical Society
Date: 15-04-2013
First cosmological results using Type Ia supernovae from the Dark Energy Survey: measurement of the Hubble constant
Publisher: Oxford University Press (OUP)
Date: 09-04-2019
DOI: 10.1093/MNRAS/STZ978
Abstract: We present an improved measurement of the Hubble constant (H0) using the ‘inverse distance ladder’ method, which adds the information from 207 Type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) at redshift 0.018 & z & 0.85 to existing distance measurements of 122 low-redshift (z & 0.07) SNe Ia (Low-z) and measurements of Baryon Acoustic Oscillations (BAOs). Whereas traditional measurements of H0 with SNe Ia use a distance ladder of parallax and Cepheid variable stars, the inverse distance ladder relies on absolute distance measurements from the BAOs to calibrate the intrinsic magnitude of the SNe Ia. We find H0 = 67.8 ± 1.3 km s−1 Mpc−1 (statistical and systematic uncertainties, 68 per cent confidence). Our measurement makes minimal assumptions about the underlying cosmological model, and our analysis was blinded to reduce confirmation bias. We examine possible systematic uncertainties and all are below the statistical uncertainties. Our H0 value is consistent with estimates derived from the Cosmic Microwave Background assuming a ΛCDM universe.
The Morphologies of Distant Galaxies. II. Classifications from the Hubble Space Telescope Medium Deep Survey
Publisher: American Astronomical Society
Date: 11-1996
DOI: 10.1086/192352
A Low-Dispersion Survey Spectrograph (LDSS-2) for the William Herschel Telescope
Publisher: IOP Publishing
Date: 09-1994
DOI: 10.1086/133471
Consistent Dynamical and Stellar Masses with Potential Light IMF in Massive Quiescent Galaxies at 3 < z < 4 Using Velocity Dispersions Measurements with MOSFIRE
Publisher: American Astronomical Society
Date: 22-02-2021
The slowly evolving role of environment in a spectroscopic survey of star formation in M* > 5 × 108 M☉ galaxies since z ̃ 1
Publisher: Oxford University Press (OUP)
Date: 17-08-2012
The distribution of satellites around massive galaxies at 1 < z < 3 in zfourge/candels
Publisher: American Astronomical Society
Date: 21-08-2014
ZFIRE
Publisher: American Astronomical Society
Date: 13-04-2017
Search for extra dimensions in diphoton events from proton–proton collisions at $\sqrt {s} = 7\,$ TeV in the ATLAS detector at the LHC
Publisher: IOP Publishing
Date: 04-04-2013
THE SFR-M∗ RELATION and EMPIRICAL STAR FORMATION HISTORIES from ZFOURGE at 0.5 < z < 4
Publisher: American Astronomical Society
Date: 27-01-2016
The Theta-z relation for HST bulges and disks out to Z approximately equal 0.8
Publisher: American Astronomical Society
Date: 10-1994
DOI: 10.1086/187573
Early Results from GLASS-JWST. VI. Extreme Rest-optical Equivalent Widths Detected in NIRISS Wide Field Slitless Spectroscopy
Publisher: American Astronomical Society
Date: 12-2022
Abstract: Wide Field Slitless Spectroscopy (WFSS) provides a powerful tool for detecting strong line emission in star-forming galaxies (SFGs) without the need for target preselection. As part of the GLASS-JWST Early Release Science (ERS) program, we leverage the near-infrared wavelength capabilities of NIRISS (1–2.2 μ m) to observe rest-optical emission lines out to z ∼ 3.4, to a depth and with a spatial resolution higher than ever before (H α to z 2.4 [O iii ]+H β to z 3.4). In this Letter we constrain the rest-frame [O III ] λ 5007 equivalent width (EW) distribution for a s le of 76 1 z 3.4 SFGs in the A2744 Hubble Frontier Field and determine an abundance fraction of extreme emission line galaxies with EW 750Å in our s le to be 12%. We determine a strong correlation between the measured H β and [O III ] λ 5007 EWs, supporting that the high [O III ] λ 5007 EW objects require massive stars in young stellar populations to generate the high-energy photons needed to doubly ionize oxygen. We extracted spectra for objects up to 2 mag fainter in the near-infrared than previous WFSS studies with the Hubble Space Telescope. Thus, this work clearly highlights the potential of JWST/NIRISS to provide high-quality WFSS data sets in crowded cluster environments.
The Sixth Data Release of the Sloan Digital Sky Survey
Publisher: American Astronomical Society
Date: 04-2008
DOI: 10.1086/524984
The differential size growth of field and cluster glaxies at z= 2.1 using the zfourge survey
Publisher: American Astronomical Society
Date: 03-06-2015
RED NUGGETS AT HIGH REDSHIFT: STRUCTURAL EVOLUTION OF QUIESCENT GALAXIES OVER 10 Gyr OF COSMIC HISTORY
Publisher: American Astronomical Society
Date: 06-09-2011
Evolved Galaxies at z > 1.5 from the Gemini Deep Deep Survey: The Formation Epoch of Massive Stellar Systems
Publisher: American Astronomical Society
Date: 13-09-2004
DOI: 10.1086/425306
The WiggleZ Dark Energy Survey: Survey design and first data release
Publisher: Oxford University Press (OUP)
Date: 21-01-2010
The Anglo-Australian Observatory 2dF facility
Publisher: Oxford University Press (OUP)
Date: 06-2002
On the Shapes and Structures of High-redshift Compact Galaxies
Publisher: American Astronomical Society
Date: 12-07-2012
Implementation and initial test results of the new Keck real time controller
Publisher: SPIE
Date: 13-12-2020
DOI: 10.1117/12.2562937
Cosmic star formation history to z = 1 from a narrow emission line-selected tunable-filter survey
Publisher: American Astronomical Society
Date: 12-2004
DOI: 10.1086/425552
A spectroscopic measurement of galaxy formation time-scales with the Redshift One LDSS3 Emission line Survey
Publisher: Oxford University Press (OUP)
Date: 24-03-2011
Promoting Correctional Integrity
Publisher: Palgrave Macmillan UK
Date: 2016
ZFIRE
Publisher: American Astronomical Society
Date: 24-08-2016
The Redshift One LDSS-3 Emission line Survey (ROLES): survey method and z ~ 1 mass-dependent star formation rate density
Publisher: Oxford University Press (OUP)
Date: 05-2010
The absence of an environmental dependence in the mass-metallicity relation at z = 2
Publisher: American Astronomical Society
Date: 02-04-2015
KiDS-i-800: comparing weak gravitational lensing measurements from same-sky surveys
Publisher: Oxford University Press (OUP)
Date: 05-04-2018
DOI: 10.1093/MNRAS/STY859
Supernova Siblings: Assessing the Consistency of Properties of Type Ia Supernovae that Share the Same Parent Galaxies
Publisher: American Astronomical Society
Date: 10-06-2020
A giant galaxy in the young Universe with a massive ring
Publisher: Springer Science and Business Media LLC
Date: 25-05-2020
Extreme Variation in Star Formation Efficiency across a Compact, Starburst Disk Galaxy
Publisher: American Astronomical Society
Date: 04-2022
Abstract: We report on the internal distribution of star formation efficiency in IRAS 08339+6517 (hereafter IRAS08), using ∼200 pc resolution CO(2 − 1) observations from NOEMA. The molecular gas depletion time changes by 2 orders-of-magnitude from disk-like values in the outer parts to less than 10 8 yr inside the half-light radius. This translates to a star formation efficiency per freefall time that also changes by 2 orders-of-magnitude, reaching 50%–100%, different than local spiral galaxies and the typical assumption of constant, low star formation efficiencies. Our target is a compact, massive disk galaxy that has a star formation rate 10× above the z = 0 main sequence Toomre Q ≈ 0.5−0.7 and high gas velocity dispersion ( σ mol ≈ 25 km s −1 ). We find that IRAS08 is similar to other rotating, starburst galaxies from the literature in the resolved Σ SFR ∝ Σ mol N relation. By combining resolved literature studies we find that the distance from the main sequence is a strong indicator of the Kennicutt-Schmidt power-law slope, with slopes of N ≈ 1.6 for starbursts from 100 to 10 4 M ⊙ pc −2 . Our target is consistent with a scenario in which violent disk instabilities drive rapid inflows of gas. It has low values of Toomre- Q , and also at all radii, the inflow timescale of the gas is less than the depletion time, which is consistent with the flat metallicity gradients in IRAS08. We consider these results in light of popular star formation theories in general observations of IRAS08 find the most tension with theories in which star formation efficiency is a constant. Our results argue for the need of high-spatial-resolution CO observations for a larger number of similar targets.
The 2-degree Field Lensing Survey: photometric redshifts from a large new training sample to r < 19.5
Publisher: Oxford University Press (OUP)
Date: 05-12-2017
Monster redshift surveys through dispersive slitless imaging: The Baryon Oscillation Probe [review article]
Publisher: Elsevier BV
Date: 11-2005
JWST UNCOVER: Extremely Red and Compact Object at z phot ≃ 7.6 Triply Imaged by A2744
Publisher: American Astronomical Society
Date: 25-07-2023
Abstract: Recent JWST/NIRCam imaging taken for the ultra-deep UNCOVER program reveals a very red dropout object at z phot ≃ 7.6, triply imaged by the galaxy cluster A2744 ( z d = 0.308). All three images are very compact, i.e., unresolved, with a delensed size upper limit of r e ≲ 35 pc. The images have apparent magnitudes of m F444W ∼ 25−26 AB, and the magnification-corrected absolute UV magnitude of the source is M UV,1450 = −16.81 ± 0.09. From the sum of observed fluxes and from a spectral energy distribution (SED) analysis, we obtain estimates of the bolometric luminosities of the source of L bol ≳ 10 43 erg s −1 and L bol ∼ 10 44 –10 46 erg s −1 , respectively. Based on its compact, point-like appearance, its position in color–color space, and the SED analysis, we tentatively conclude that this object is a UV-faint dust-obscured quasar-like object, i.e., an active galactic nucleus at high redshift. We also discuss other alternative origins for the object’s emission features, including a massive star cluster, Population III, supermassive, or dark stars, or a direct-collapse black hole. Although populations of red galaxies at similar photometric redshifts have been detected with JWST, this object is unique in that its high-redshift nature is corroborated geometrically by lensing, that it is unresolved despite being magnified—and thus intrinsically even more compact—and that it occupies notably distinct regions in both size–luminosity and color–color space. Planned UNCOVER JWST/NIRSpec observations, scheduled in Cycle 1, will enable a more detailed analysis of this object.
The Morphology of Faint Galaxies in Medium Deep Survey Images Using WFPC2
Publisher: American Astronomical Society
Date: 11-1994
DOI: 10.1086/187584
2dFLenS and KiDS: determining source redshift distributions with cross-correlations
Publisher: Oxford University Press (OUP)
Date: 23-11-2017
ATLAS probe for the study of galaxy evolution with 300,000,000 galaxy spectra
Publisher: SPIE
Date: 22-08-2018
DOI: 10.1117/12.2313082
LensingETC: A Tool to Optimize Multifilter Imaging Campaigns of Galaxy-scale Strong Lensing Systems
Publisher: American Astronomical Society
Date: 10-2022
Abstract: Imaging data is the principal observable required to use galaxy-scale strong lensing in a multitude of applications in extragalactic astrophysics and cosmology. In this paper, we develop Lensing Exposure Time Calculator (L ensing ETC jshajib/LensingETC ) to optimize the efficiency of telescope-time usage when planning multifilter imaging c aigns for galaxy-scale strong lenses. This tool simulates realistic data tailored to specified instrument characteristics and then automatically models them to assess the power of the data in constraining lens model parameters. We demonstrate a use case of this tool by optimizing a two-filter observing strategy (in the IR and ultraviolet-visual (UVIS)) within the limited exposure time per system allowed by a Hubble Space Telescope (HST) Snapshot program. We find that higher resolution is more advantageous to gain constraining power on the lensing observables, when there is a trade-off between signal-to-noise ratio and resolution for ex le, between the UVIS and IR filters of the HST. We also find that, whereas a point-spread function (PSF) with sub-Nyquist s ling allows the s le mean for a model parameter to be robustly recovered for both galaxy–galaxy and point-source lensing systems, a sub-Nyquist-s led PSF introduces a larger scatter than a Nyquist-s led one in the deviation from the ground truth for point-source lens systems.
THE REDMAPPER GALAXY CLUSTER CATALOG FROM DES SCIENCE VERIFICATION DATA
Publisher: American Astronomical Society
Date: 02-05-2016
Integrated and Resolved Dust Attenuation in Clumpy Star-Forming Galaxies at 0.07 < z < 0.14
Publisher: Oxford University Press (OUP)
Date: 17-11-2016
Early Results from GLASS-JWST. XIX. A High Density of Bright Galaxies at z ≈ 10 in the A2744 Region
Publisher: American Astronomical Society
Date: 05-2023
Abstract: We report the detection of a high density of redshift z ≈ 10 galaxies behind the foreground cluster A2744, selected from imaging data obtained recently with NIRCam on board JWST by three programs—GLASS-JWST, UNCOVER, and DDT#2756. To ensure robust estimates of the lensing magnification μ , we use an improved version of our model that exploits the first epoch of NIRCam images and newly obtained MUSE spectra and avoids regions with μ 5 where the uncertainty may be higher. We detect seven bright z ≈ 10 galaxies with demagnified rest frame −22 ≲ M UV ≲ −19 mag, over an area of ∼37 arcmin 2 . Taking into account photometric incompleteness and the effects of lensing on luminosity and cosmological volume, we find that the density of z ≈ 10 galaxies in the field is about 10× (3×) larger than the average at M UV ≈ −21 ( −20) mag reported so far. The density is even higher when considering only the GLASS-JWST data, which are the deepest and the least affected by magnification and incompleteness. The GLASS-JWST field contains five out of seven galaxies, distributed along an apparent filamentary structure of 2 Mpc in projected length, and includes a close pair of candidates with M UV −20 mag having a projected separation of only 16 kpc. These findings suggest the presence of a z ≈ 10 overdensity in the field. In addition to providing excellent targets for efficient spectroscopic follow-up observations, our study confirms the high density of bright galaxies observed in early JWST observations but calls for multiple surveys along independent lines of sight to achieve an unbiased estimate of their average density and a first estimate of their clustering.
Gemini Deep Deep Survey. VI. Massive Hδ‐strong Galaxies atz≃ 1
Publisher: American Astronomical Society
Date: 05-2006
DOI: 10.1086/500005
The Sloan Digital Sky Survey: The Cosmic Spectrum and Star Formation History
Publisher: American Astronomical Society
Date: 10-04-2003
DOI: 10.1086/368161
WiggleZ Dark Energy Survey: Cosmological neutrino mass constraint from blue high-redshift galaxies
Publisher: American Physical Society (APS)
Date: 23-04-2012
The host galaxies of 106 rapidly evolving transients discovered by the Dark Energy Survey
Publisher: Oxford University Press (OUP)
Date: 17-08-2020
Abstract: Rapidly evolving transients (RETs), also termed fast blue optical transients, are a recently discovered group of astrophysical events that display rapid luminosity evolution. RETs typically rise to peak in less than 10 d and fade within 30, a time-scale unlikely to be compatible with the decay of Nickel-56 that drives conventional supernovae (SNe). Their peak luminosity spans a range of −15 & Mg & −22.5, with some events observed at redshifts greater than 1. Their evolution on fast time-scales has hindered high-quality follow-up observations, and thus their origin and explosion/emission mechanism remains unexplained. In this paper, we present the largest s le of RETs to date, comprising 106 objects discovered by the Dark Energy Survey, and perform the most comprehensive analysis of RET host galaxies. Using deep-stacked photometry and emission lines from OzDES spectroscopy, we derive stellar masses and star formation rates (SFRs) for 49 host galaxies, and metallicities ([O/H]) for 37. We find that RETs explode exclusively in star-forming galaxies and are thus likely associated with massive stars. Comparing RET hosts to s les of host galaxies of other explosive transients as well as field galaxies, we find that RETs prefer galaxies with high specific SFRs (〈log (sSFR)〉 ∼ −9.6), indicating a link to young stellar populations, similar to stripped-envelope SNe. RET hosts appear to show a lack of chemical enrichment, their metallicities akin to long-duration gamma-ray bursts and superluminous SN host galaxies (〈12 + log (O/H)〉 ∼ 9.4). There are no clear relationships between mass or SFR of the host galaxies and the peak magnitudes or decline rates of the transients themselves.
Finding high-redshift strong lenses in DES using convolutional neural networks
Publisher: Oxford University Press (OUP)
Date: 25-01-2019
DOI: 10.1093/MNRAS/STZ272
An imaging K-band survey - I. The catalogue, star and galaxy counts
Publisher: Oxford University Press (OUP)
Date: 1994
A faint galaxy redshift survey to B=24
Publisher: Oxford University Press (OUP)
Date: 03-1995
Quasar Accretion Disk Sizes from Continuum Reverberation Mapping in the DES Standard-star Fields
Publisher: American Astronomical Society
Date: 16-01-2020
The SAMI Galaxy Survey: trends in [α/Fe] as a function of morphology and environment
Publisher: Oxford University Press (OUP)
Date: 12-2021
Abstract: We present a new set of index-based measurements of [α/Fe] for a s le of 2093 galaxies in the SAMI Galaxy Survey. Following earlier work, we fit a global relation between [α/Fe] and the galaxy velocity dispersion σ for red sequence galaxies, $[\\alpha /\\text{Fe}]=(0.378\\pm 0.009)\\rm {log}_{10}\\left(\\sigma /100\\right)+(0.155\\pm 0.003)$. We observe a correlation between the residuals and the local environmental surface density, whereas no such relation exists for blue cloud galaxies. In the full s le, we find that elliptical galaxies in high-density environments are α-enhanced by up to 0.057 ± 0.014 dex at velocity dispersions σ & 100 km s−1, compared with those in low-density environments. This α-enhancement is morphology-dependent, with the offset decreasing along the Hubble sequence towards spirals, which have an offset of 0.019 ± 0.014 dex. At low velocity dispersion and controlling for morphology, we estimate that star formation in high-density environments is truncated ∼1 Gyr earlier than in low-density environments. For elliptical galaxies only, we find support for a parabolic relationship between [α/Fe] and σ, with an environmental α-enhancement of at least 0.03 dex. This suggests strong contributions from both environment and mass-based quenching mechanisms. However, there is no evidence for this behaviour in later morphological types.
A small-area faint KX redshift survey for QSOs in the ESO Imaging Survey Chandra Deep Field South
Publisher: Oxford University Press (OUP)
Date: 11-2001
Early Results From GLASS-JWST. XII. The Morphology of Galaxies at the Epoch of Reionization
Publisher: American Astronomical Society
Date: 2023
Abstract: Star-forming galaxies can exhibit strong morphological differences between the rest-frame far-UV and optical, reflecting inhomogeneities in star formation and dust attenuation. We exploit deep, high-resolution, NIRCAM seven-band observations to take a first look at the morphology of galaxies in the epoch of reionization ( z 7), and its variation in the rest-frame wavelength range between Ly α and 6000–4000 Å, at z = 7–12. We find no dramatic variations in morphology with wavelength—of the kind that would have overturned anything we have learned from the Hubble Space Telescope. No significant trends between morphology and wavelengths are detected using standard quantitative morphology statistics. We detect signatures of mergers/interactions in 4/19 galaxies. Our results are consistent with a scenario in which Lyman-break galaxies—observed when the universe is only 400–800 Myr old—are growing via a combination of rapid, galaxy-scale star formation supplemented by the accretion of star-forming clumps and interactions.
A spectroscopic measure of the star formation rate density in dwarf galaxies at z ~ 1
Publisher: Oxford University Press (OUP)
Date: 05-2009
A Study of Quasar Selection in the Supernova Fields of the Dark Energy Survey
Publisher: American Astronomical Society
Date: 14-02-2017
Measurement of the centrality dependence of J / ψ
Publisher:
Elsevier BV
Date:
03-2011
Publisher: Elsevier BV
Date: 03-2011
Four faint T dwarfs from the UKIRT Infrared Deep Sky Survey (UKIDSS) Southern Stripe
Publisher: Oxford University Press (OUP)
Date: 03-2008
The Gemini Deep Deep Survey. VIII. When Did Early‐Type Galaxies Form?
Publisher: American Astronomical Society
Date: 11-2007
DOI: 10.1086/521138
Reconstructing the Observed Ionizing Photon Production Efficiency at z ∼ 2 Using Stellar Population Models
Publisher: American Astronomical Society
Date: 05-02-2020
Implications for the Hubble Constant from the First Seven Supernovae at [CLC][ITAL]z[/ITAL][/CLC] ≥ 0.35
Publisher: American Astronomical Society
Date: 20-02-1997
DOI: 10.1086/310507
Three Lyα Emitters at z ~ 6: Early GMOS/Gemini Data from the GLARE Project
Publisher: American Astronomical Society
Date: 23-02-2004
DOI: 10.1086/383523
Dust properties of clumpy disc galaxies at z ̃ 1.3 with Herschel-SPIRE
Publisher: Oxford University Press (OUP)
Date: 18-09-2013
The SAMI galaxy survey: gas velocity dispersions in low-z star-forming galaxies and the drivers of turbulence
Publisher: Oxford University Press (OUP)
Date: 20-05-2020
Abstract: We infer the intrinsic ionized gas kinematics for 383 star-forming galaxies across a range of integrated star formation rates (SFR ∈ [10−3, 102] M⊙ yr−1) at z ≲ 0.1 using a consistent 3D forward-modelling technique. The total s le is a combination of galaxies from the Sydney-AAO Multiobject Integral field Spectrograph (SAMI) Galaxy survey and DYnamics of Newly Assembled Massive Objects survey. For typical low-z galaxies taken from the SAMI Galaxy Survey, we find the vertical velocity dispersion (σv,z) to be positively correlated with measures of SFR, stellar mass, H i gas mass, and rotational velocity. The greatest correlation is with SFR surface density (ΣSFR). Using the total s le, we find σv,z increases slowly as a function of integrated SFR in the range SFR ∈ [10−3, 1] M⊙ yr−1 from 17 ± 3 to 24 ± 5 km s−1 followed by a steeper increase up to σv,z ∼80 km s−1 for SFR ≳ 1 M⊙ yr−1. This is consistent with recent theoretical models that suggest a σv,z floor driven by star formation feedback processes with an upturn in σv,z at higher SFR driven by gravitational transport of gas through the disc.
CO Excitation in High-z Main-sequence Analogues
Publisher: American Astronomical Society
Date: 03-2023
Abstract: The spectral line energy distribution of carbon monoxide contains information about the physical conditions of the star-forming molecular hydrogen gas however, the relation to local radiation field properties is poorly constrained. Using ∼1–2 kpc scale Atacama Large Millimeter Array observations of CO(3−2) and CO(4−3), we characterize the CO(4−3)/CO(3−2) line ratios of local analogues of main-sequence galaxies at z ∼ 1–2, drawn from the DYnamics of Newly Assembled Massive Objects (DYNAMO) s le. We measure CO(4−3)/CO(3−2) across the disk of each galaxy and find a median line ratio of R 43 = 0.54 − 0.15 + 0.16 for the s le. This is higher than literature estimates of local star-forming galaxies and is consistent with multiple lines of evidence that indicate DYNAMO galaxies, despite residing in the local universe, resemble main-sequence galaxies at z ∼ 1–2. Comparing with existing lower-resolution CO(1−0) observations, we find R 41 and R 31 values in the range ∼0.2–0.3 and ∼0.4–0.8, respectively. We combine our kiloparsec-scale resolved line ratio measurements with Hubble Space Telescope observations of H α to investigate the relation to the star formation rate surface density and compare this relation to expectations from models. We find increasing CO(4−3)/CO(3−2) with increasing star formation rate surface density however, models overpredict the line ratios across the range of star formation rate surface densities we probe, in particular at the lower range. Finally, Stratospheric Observatory for Infrared Astronomy observations with the High-resolution Airborne Wideband Camera Plus and Field-Imaging Far-Infrared Line Spectrometer reveal low dust temperatures and no deficit of [C ii ] emission with respect to the total infrared luminosity.
ATLAS probe: Breakthrough science of galaxy evolution, cosmology, Milky Way, and the Solar System
Publisher: Cambridge University Press (CUP)
Date: 2019
DOI: 10.1017/PASA.2019.5
Abstract: Astrophysics Telescope for Large Area Spectroscopy Probe is a concept for a National Aeronautics and Space Administration probe-class space mission that will achieve ground-breaking science in the fields of galaxy evolution, cosmology, Milky Way, and the Solar System. It is the follow-up space mission to Wide Field Infrared Survey Telescope (WFIRST), boosting its scientific return by obtaining deep 1–4 μm slit spectroscopy for ∼70% of all galaxies imaged by the ∼2 000 deg 2 WFIRST High Latitude Survey at z 0.5. Astrophysics Telescope for Large Area Spectroscopy will measure accurate and precise redshifts for ∼200 M galaxies out to z 7, and deliver spectra that enable a wide range of diagnostic studies of the physical properties of galaxies over most of cosmic history. Astrophysics Telescope for Large Area Spectroscopy Probe and WFIRST together will produce a 3D map of the Universe over 2 000 deg 2 , the definitive data sets for studying galaxy evolution, probing dark matter, dark energy and modifications of General Relativity, and quantifying the 3D structure and stellar content of the Milky Way. Astrophysics Telescope for Large Area Spectroscopy Probe science spans four broad categories: (1) Revolutionising galaxy evolution studies by tracing the relation between galaxies and dark matter from galaxy groups to cosmic voids and filaments, from the epoch of reionisation through the peak era of galaxy assembly (2) Opening a new window into the dark Universe by weighing the dark matter filaments using 3D weak lensing with spectroscopic redshifts, and obtaining definitive measurements of dark energy and modification of General Relativity using galaxy clustering (3) Probing the Milky Way’s dust-enshrouded regions, reaching the far side of our Galaxy and (4) Exploring the formation history of the outer Solar System by characterising Kuiper Belt Objects. Astrophysics Telescope for Large Area Spectroscopy Probe is a 1.5 m telescope with a field of view of 0.4 deg 2 , and uses digital micro-mirror devices as slit selectors. It has a spectroscopic resolution of R = 1 000, and a wavelength range of 1–4 μm. The lack of slit spectroscopy from space over a wide field of view is the obvious gap in current and planned future space missions Astrophysics Telescope for Large Area Spectroscopy fills this big gap with an unprecedented spectroscopic capability based on digital micro-mirror devices (with an estimated spectroscopic multiplex factor greater than 5 000). Astrophysics Telescope for Large Area Spectroscopy is designed to fit within the National Aeronautics and Space Administration probe-class space mission cost envelope it has a single instrument, a telescope aperture that allows for a lighter launch vehicle, and mature technology (we have identified a path for digital micro-mirror devices to reach Technology Readiness Level 6 within 2 yr). Astrophysics Telescope for Large Area Spectroscopy Probe will lead to transformative science over the entire range of astrophysics: from galaxy evolution to the dark Universe, from Solar System objects to the dusty regions of the Milky Way.
Quasar Accretion Disk Sizes from Continuum Reverberation Mapping from the Dark Energy Survey
Publisher: American Astronomical Society
Date: 30-07-2018
From peculiar morphologies to Hubble-type spirals: the relation between galaxy dynamics and morphology in star-forming galaxies at z ∼ 1.5
Publisher: Oxford University Press (OUP)
Date: 23-12-2019
Abstract: We present an analysis of the gas dynamics of star-forming galaxies at z ∼ 1.5 using data from the KMOS Galaxy Evolution Survey. We quantify the morphology of the galaxies using HSTcandels imaging parametrically and non-parametrically. We combine the H α dynamics from KMOS with the high-resolution imaging to derive the relation between stellar mass (M*) and stellar specific angular momentum (j*). We show that high-redshift star-forming galaxies at z ∼ 1.5 follow a power-law trend in specific stellar angular momentum with stellar mass similar to that of local late-type galaxies of the form j* ∝ M$_*^{0.53\\, \\pm \\, 0.10}$. The highest specific angular momentum galaxies are mostly disc-like, although generally both peculiar morphologies and disc-like systems are found across the sequence of specific angular momentum at a fixed stellar mass. We explore the scatter within the j* – M* plane and its correlation with both the integrated dynamical properties of a galaxy (e.g. velocity dispersion, Toomre Qg, H α star formation rate surface density ΣSFR) and its parametrized rest-frame UV / optical morphology (e.g. Sérsic index, bulge to total ratio, clumpiness, asymmetry, and concentration). We establish that the position in the j* – M* plane is strongly correlated with the star-formation surface density and the clumpiness of the stellar light distribution. Galaxies with peculiar rest-frame UV / optical morphologies have comparable specific angular momentum to disc- dominated galaxies of the same stellar mass, but are clumpier and have higher star formation rate surface densities. We propose that the peculiar morphologies in high-redshift systems are driven by higher star formation rate surface densities and higher gas fractions leading to a more clumpy interstellar medium.
High star formation rates as the origin of turbulence in early and modern disk galaxies
Publisher: Springer Science and Business Media LLC
Date: 10-2010
DOI: 10.1038/NATURE09452
Abstract: Observations of star formation and kinematics in early galaxies at high spatial and spectral resolution have shown that two-thirds are massive rotating disk galaxies, with the remainder being less massive non-rotating objects. The line-of-sight-averaged velocity dispersions are typically five times higher than in today's disk galaxies. This suggests that gravitationally unstable, gas-rich disks in the early Universe are fuelled by cold, dense accreting gas flowing along cosmic filaments and penetrating hot galactic gas halos. These accreting flows, however, have not been observed, and cosmic accretion cannot power the observed level of turbulence. Here we report observations of a s le of rare, high-velocity-dispersion disk galaxies in the nearby Universe where cold accretion is unlikely to drive their high star formation rates. We find that their velocity dispersions are correlated with their star formation rates, but not their masses or gas fractions, which suggests that star formation is the energetic driver of galaxy disk turbulence at all cosmic epochs.
On the galaxy stellar mass function, the mass–metallicity relation and the implied baryonic mass function
Publisher: Oxford University Press (OUP)
Date: 06-2008
ANGULAR MOMENTUM REGULATES ATOMIC GAS FRACTIONS of GALACTIC DISKS
Publisher: American Astronomical Society
Date: 20-06-2016
The Subaru FMOS galaxy redshift survey (FastSound). I. Overview of the survey targeting Hα emitters at z∼1.4
Publisher: Oxford University Press (OUP)
Date: 23-06-2015
DOI: 10.1093/PASJ/PSV044
The Gemini Deep Deep Survey. VII. The Redshift Evolution of the Mass‐Metallicity Relation
Publisher: American Astronomical Society
Date: 10-12-2005
DOI: 10.1086/497331
ZFIRE
Publisher: American Astronomical Society
Date: 16-09-2015
KROSS–SAMI: a direct IFS comparison of the Tully–Fisher relation across 8 Gyr sincez ≈ 1
Publisher: Oxford University Press (OUP)
Date: 17-10-2018
Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies
Publisher: EDP Sciences
Date: 10-2018
DOI: 10.1051/0004-6361/201833070
Abstract: We present Keck–MOSFIRE H and K spectra for a s le of 24 candidate quiescent galaxies at 3 z 4, identified from their rest-frame U V J colors and photometric redshifts in the ZFOURGE and 3DHST surveys. With median integration times of one hour in H and five in K , we obtain spectroscopic redshifts for half of the s le, using either Balmer absorption lines or nebular emission lines. We confirm the high accuracy of the photometric redshifts for this spectroscopically-confirmed s le, with a median | Z phot − Z spec |/(1 + Z spec ) of 1.2%. Two galaxies turn out to be dusty H α emitters at lower redshifts ( z 2.5), and these are the only two detected in the sub-mm with ALMA. High equivalent-width [O III ] emission is observed in two galaxies, contributing up to 30% of the K -band flux and mimicking the U V J colors of an old stellar population. This implies a failure rate of only 20% for the U V J selection at these redshifts. Lastly, Balmer absorption features are identified in four galaxies, among the brightest of the s le, confirming the absence of OB stars. We then modeled the spectra and photometry of all quiescent galaxies with a wide range of star-formation histories. We find specific star-formation rates (sSFR) lower than 0.15 Gyr −1 (a factor of ten below the main sequence) for all but one galaxy, and lower than 0.01 Gyr −1 for half of the s le. These values are consistent with the observed Hβ and [O II ] luminosities, and the ALMA non-detections. The implied formation histories reveal that these galaxies have quenched on average 300 Myr prior to being observed, between z = 3.5 and 5, and that half of their stars were formed by z ∼ 5.5 with a mean SFR ~ 300 M ⊙ yr −1 . We finally compared the U V J selection to a selection based instead on the sSFR, as measured from the photometry. We find that galaxies a factor of ten below the main sequence are 40% more numerous than U V J -selected quiescent galaxies, implying that the U V J selection is pure but incomplete. Current models fail at reproducing our observations, and underestimate either the number density of quiescent galaxies by more than an order of magnitude, or the duration of their quiescence by a factor two. Overall, these results confirm the existence of an unexpected population of quiescent galaxies at z 3, and offer the first insights on their formation histories.
Evidence for a Nonuniversal Stellar Initial Mass Function from the Integrated Properties of SDSS Galaxies
Publisher: American Astronomical Society
Date: 03-2008
DOI: 10.1086/524095
Dark Energy Survey Year 1 Results: redshift distributions of the weak-lensing source galaxies
Publisher: Oxford University Press (OUP)
Date: 18-04-2018
DOI: 10.1093/MNRAS/STY957
DYNAMO-HST survey
Publisher: Oxford University Press (OUP)
Date: 14-09-2017
Jekyll & Hyde: quiescence and extreme obscuration in a pair of massive galaxies 1.5 Gyr after the Big Bang
Publisher: EDP Sciences
Date: 03-2018
DOI: 10.1051/0004-6361/201731917
Abstract: We obtained ALMA spectroscopy and deep imaging to investigate the origin of the unexpected sub-millimeter emission toward the most distant quiescent galaxy known to date, ZF-COSMOS-20115 at z = 3.717. We show here that this sub-millimeter emission is produced by another massive ( M * ~ 10 11 M ⊙ ), compact ( r 1∕2 = 0.67 ± 0.14 kpc) and extremely obscured galaxy ( A V ~ 3.5), located only 0.43 ′′ (3.1 kpc) away from the quiescent galaxy. We dub the quiescent and dusty galaxies Jekyll and Hyde, respectively. No dust emission is detected at the location of the quiescent galaxy, implying SFR 13 M ⊙ yr −1 which is the most stringent upper limit ever obtained for a quiescent galaxy at these redshifts. The two sources are spectroscopically confirmed to lie at the same redshift thanks to the detection of [C II ] 158 in Hyde ( z = 3.709), which provides one the few robust redshifts for a highly-obscured “ H -dropout” galaxy ( H − [4.5] = 5.1 ± 0.8). The [C II ] line shows a clear rotating-disk velocity profile which is blueshifted compared to the Balmer lines of Jekyll by 549 ± 60 km s −1 , demonstrating that it is produced by another galaxy. Careful de-blending of the Spitzer imaging confirms the existence of this new massive galaxy, and its non-detection in the Hubble images requires extremely red colors and strong attenuation by dust. Full modeling of the UV-to-far-IR emission of both galaxies shows that Jekyll has fully quenched at least 200Myr prior to observation and still presents a challenge for models, while Hyde only harbors moderate star-formation with SFR ≲ 120 M ⊙ yr −1 , and is located at least a factor 1.4 below the z ~ 4 main sequence. Hyde could also have stopped forming stars less than 200 Myr before being observed this interpretation is also suggested by its compactness comparable to that of z ~ 4 quiescent galaxies and its low [C II ]/FIR ratio, but significant on-going star-formation cannot be ruled out. Lastly, we find that despite its moderate SFR, Hyde hosts a dense reservoir of gas comparable to that of the most extreme starbursts. This suggests that whatever mechanism has stopped or reduced its star-formation must have done so without expelling the gas outside of the galaxy. Because of their surprisingly similar mass, compactness, environment and star-formation history, we argue that Jekyll and Hyde can be seen as two stages of the same quenching process, and provide a unique laboratory to study this poorly understood phenomenon.
Hubble Space TelescopeImaging of the CFRS and LDSS Redshift Surveys. I. Morphological Properties
Publisher: American Astronomical Society
Date: 20-05-1998
DOI: 10.1086/305621
ZFIRE: Measuring Electron Density with [O ii] as a Function of Environment at z = 1.62
Publisher: American Astronomical Society
Date: 31-03-2020
KAOS: kilo-aperture optical spectrograph
Publisher: SPIE
Date: 30-09-2004
DOI: 10.1117/12.550287
The 2-degree Field Lensing Survey: design and clustering measurements
Publisher: Oxford University Press (OUP)
Date: 09-08-2016
A UV-visible prime focus camera for the Keck telescopes
Publisher: SPIE
Date: 03-01-2020
DOI: 10.1117/12.2540717
ZFIRE: The Beginning of the End for Massive Galaxies at z ∼ 2 and Why Environment Matters
Publisher: American Astronomical Society
Date: 09-2021
A NEAR-INFRARED EXCESS IN THE CONTINUUM OF HIGH-REDSHIFT GALAXIES: A TRACER OF STAR FORMATION AND CIRCUMSTELLAR DISKS?
Publisher: American Astronomical Society
Date: 09-11-2009
KECK/MOSFIRE SPECTROSCOPIC CONFIRMATION OF A VIRGO-LIKE CLUSTER ANCESTOR AT z = 2.095
Publisher: American Astronomical Society
Date: 17-10-2014
Hubble Space Telescope imaging of the CFRS and LDSS redshift surveys--IV. Influence of mergers in the evolution of faint field galaxies from z 1
Publisher: Oxford University Press (OUP)
Date: 21-01-2000
OBSERVATION AND CONFIRMATION OF SIX STRONG-LENSING SYSTEMS IN THE DARK ENERGY SURVEY SCIENCE VERIFICATION DATA
Publisher: American Astronomical Society
Date: 05-08-2016
Measuring the 2D baryon acoustic oscillation signal of galaxies in WiggleZ: cosmological constraints
Publisher: Oxford University Press (OUP)
Date: 23-10-2017
The SAMI Galaxy Survey: Asymmetry in gas kinematics and its links to stellar mass and star formation
Publisher: Oxford University Press (OUP)
Date: 12-10-2017
Galaxy stellar mass functions from zfourge/candels
Publisher: American Astronomical Society
Date: 20-02-2014
The Bimodal Galaxy Color Distribution: Dependence on Luminosity and Environment
Publisher: American Astronomical Society
Date: 30-09-2004
DOI: 10.1086/426079
The first sample of spectroscopically confirmed ultra-compact massive galaxies in the Kilo Degree Survey
Publisher: Oxford University Press (OUP)
Date: 20-09-2018
UV to IR Luminosities and Dust Attenuation Determined from ~4000 K-selected Galaxies at 1 〈 z 〈 3 in the ZFOURGE Survey
Publisher: American Astronomical Society
Date: 11-02-2016
HSTHα grism spectroscopy of ROLES: a flatter low-mass slope for thez ∼ 1 SSFR–mass relation
Publisher: Oxford University Press (OUP)
Date: 15-12-2016
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View Funded ActivityDiscovery Projects - Grant ID: DP130101460
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Amount: $335,000.00
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View Funded ActivityLinkage - International - Grant ID: LX0989763
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Amount: $58,000.00
Funder: Australian Research Council
View Funded ActivityDiscovery Projects - Grant ID: DP0774469
Start Date: 2007
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Amount: $350,000.00
Funder: Australian Research Council
View Funded ActivitySuper Science Fellowships - Grant ID: FS110200007
Start Date: 08-2011
End Date: 11-2014
Amount: $556,800.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE120100023
Start Date: 01-2012
End Date: 12-2012
Amount: $185,000.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE150100024
Start Date: 06-2015
End Date: 12-2017
Amount: $760,000.00
Funder: Australian Research Council
View Funded ActivityDiscovery Projects - Grant ID: DP1094370
Start Date: 2010
End Date: 12-2013
Amount: $330,000.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE100100164
Start Date: 11-2010
End Date: 11-2010
Amount: $500,000.00
Funder: Australian Research Council
View Funded ActivityDiscovery Projects - Grant ID: DP130101667
Start Date: 2013
End Date: 12-2016
Amount: $341,000.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE150100055
Start Date: 04-2015
End Date: 12-2016
Amount: $560,000.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE130100198
Start Date: 07-2013
End Date: 12-2014
Amount: $315,000.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE140100013
Start Date: 2014
End Date: 12-2016
Amount: $300,000.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE220100007
Start Date: 07-2024
End Date: 06-2027
Amount: $1,275,295.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE160100145
Start Date: 06-2016
End Date: 09-2017
Amount: $430,000.00
Funder: Australian Research Council
View Funded ActivityLinkage Infrastructure, Equipment And Facilities - Grant ID: LE110100030
Start Date: 05-2011
End Date: 12-2014
Amount: $350,000.00
Funder: Australian Research Council
View Funded ActivityDiscovery Projects - Grant ID: DP0772084
Start Date: 2007
End Date: 12-2010
Amount: $588,000.00
Funder: Australian Research Council
View Funded ActivityDiscovery Projects - Grant ID: DP1093738
Start Date: 2010
End Date: 12-2013
Amount: $560,000.00
Funder: Australian Research Council
View Funded ActivitySpecial Research Initiatives - Grant ID: SR0354527
Start Date: 05-2004
End Date: 12-2004
Amount: $10,000.00
Funder: Australian Research Council
View Funded Activity