ORCID Profile
0000-0002-5542-1940
Current Organisation
Institut Teknologi Bandung
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Publisher: Springer India
Date: 2016
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940826
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940824
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940825
Publisher: Elsevier BV
Date: 05-2008
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4724129
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940823
Publisher: IOP Publishing
Date: 2019
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940821
Publisher: EDP Sciences
Date: 28-10-2016
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4724165
Publisher: Oxford University Press (OUP)
Date: 04-2017
DOI: 10.1093/MNRAS/STX808
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4724120
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4724167
Publisher: IOP Publishing
Date: 04-2018
Publisher: Springer Science and Business Media LLC
Date: 09-12-2016
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 04-2016
Publisher: University of Zielona Góra, Poland
Date: 2010
DOI: 10.7151/DMGT.1519
Publisher: Oxford University Press (OUP)
Date: 20-09-2019
Abstract: SIGNALS, the Star formation, Ionized Gas, and Nebular Abundances Legacy Survey, is a large observing programme designed to investigate massive star formation and H ii regions in a s le of local extended galaxies. The programme will use the imaging Fourier transform spectrograph SITELLE at the Canada–France–Hawaii Telescope. Over 355 h (54.7 nights) have been allocated beginning in fall 2018 for eight consecutive semesters. Once completed, SIGNALS will provide a statistically reliable laboratory to investigate massive star formation, including over 50 000 resolved H ii regions: the largest, most complete, and homogeneous data base of spectroscopically and spatially resolved extragalactic H ii regions ever assembled. For each field observed, three datacubes covering the spectral bands of the filters SN1 (363–386 nm), SN2 (482–513 nm), and SN3 (647–685 nm) are gathered. The spectral resolution selected for each spectral band is 1000, 1000, and 5000, respectively. As defined, the project s le will facilitate the study of small-scale nebular physics and many other phenomena linked to star formation at a mean spatial resolution of ∼20 pc. This survey also has considerable legacy value for additional topics, including planetary nebulae, diffuse ionized gas, and supernova remnants. The purpose of this paper is to present a general outlook of the survey, notably the observing strategy, galaxy s le, and science requirements.
Publisher: Elsevier BV
Date: 02-2013
Publisher: EDP Sciences
Date: 02-2022
DOI: 10.1051/0004-6361/202141888
Abstract: Context. Voids are the most under-dense large-scale regions in the Universe. Galaxies inhabiting voids are one of the keys for understanding the intrinsic processes of galaxy evolution, as external factors such as multiple galaxy mergers or a dense self-collapsing environment are negligible. Aims. We present the first molecular gas mass survey of void galaxies. We compare these new data together with data for the atomic gas mass ( M H I ) and star formation rate (SFR) from the literature to those of galaxies in filaments and walls in order to better understand how molecular gas and star formation are related to the large-scale environment. Methods. We observed at the IRAM 30 m telescope the CO(1−0) and CO(2−1) emission of 20 void galaxies selected from the Void Galaxy Survey, with a stellar mass range from 10 8.5 to 10 10.3 M ⊙ . We detected 15 objects in at least one CO line. We compared the molecular gas mass ( M H 2 ), the star formation efficiency (SFE = SFR/ M H 2 ), the atomic gas mass, the molecular-to-atomic gas mass ratio, and the specific star formation rate (sSFR) of the void galaxies with two control s les of galaxies in filaments and walls, selected from xCOLD GASS and EDGE-CALIFA, for different stellar mass bins and taking the star formation activity into account. Results. In general, we do not find any significant differences between void galaxies and the control s le. In particular, we do not find any evidence for a difference in the molecular gas mass or molecular gas mass fraction. For the other parameters (SFE, atomic gas mass, molecular-to-atomic gas mass ratio, and sSFR), we also find similar (within the errors) mean values between void and filament and wall galaxies when the s le is limited to star-forming galaxies. We find no evidence for an enhanced sSFR in void galaxies. Some tentative differences emerge when trends with stellar mass are studied: The SFE of void galaxies might be lower than in filament and wall galaxies for low stellar masses, and there might be a trend of increasing deficiency in the HI content in void galaxies compared to galaxies in filaments and walls for higher stellar masses, accompanied by an increase in the molecular-to-atomic gas mass ratio. However, all trends with stellar mass are based on a low number of galaxies and need to be confirmed for a larger s le. Conclusions. The results for the molecular gas mass for a s le of 20 voids galaxies allowed us to make a statistical comparison to galaxies in filaments and walls for the first time. We do not find any significant differences of the molecular gas properties and the SFE, but we note that a larger s le is necessary to confirm this and be sensitive to subtle trends.
Publisher: EDP Sciences
Date: 03-2022
DOI: 10.1051/0004-6361/202141568
Abstract: We use type Ia supernova (SN Ia) data obtained by the Sloan Digital Sky Survey-II Supernova Survey (SDSS-II SNS) in combination with the publicly available SDSS DR16 fiber spectroscopy of supernova (SN) host galaxies to correlate SN Ia light-curve parameters and Hubble residuals with several host galaxy properties. Fixed-aperture fiber spectroscopy suffers from aperture effects: the fraction of the galaxy covered by the fiber varies depending on its projected size on the sky, and thus measured properties are not representative of the whole galaxy. The advent of integral field spectroscopy has provided a way to correct the missing light, by studying how these galaxy parameters change with the aperture size. Here we study how the standard SN host galaxy relations change once global host galaxy parameters are corrected for aperture effects. We recover previous trends on SN Hubble residuals with host galaxy properties, but we find that discarding objects with poor fiber coverage instead of correcting for aperture loss introduces biases into the s le that affect SN host galaxy relations. The net effect of applying the commonly used g -band fraction criterion is that intrinsically faint SNe Ia in high-mass galaxies are discarded, thus artificially increasing the height of the mass step by 0.02 mag and its significance. Current and next-generation fixed-aperture fiber-spectroscopy surveys, such as OzDES, DESI, or TiDES with 4MOST, that aim to study SN and galaxy correlations must consider, and correct for, these effects.
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 2011
Publisher: International Journal of Technology
Date: 30-12-2015
Publisher: Springer Science and Business Media LLC
Date: 05-01-2021
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4724133
Publisher: Springer Science and Business Media LLC
Date: 12-2002
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4726159
Publisher: Elsevier BV
Date: 11-2010
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 08-10-2016
Publisher: Springer International Publishing
Date: 2016
Publisher: Elsevier BV
Date: 2015
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 04-2017
Publisher: Elsevier BV
Date: 05-2005
Publisher: Academic Publications
Date: 15-06-2015
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 04-2015
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 2004
Publisher: AIP Publishing LLC
Date: 2014
DOI: 10.1063/1.4868770
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940807
Publisher: Elsevier BV
Date: 2015
Publisher: Elsevier BV
Date: 2015
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940802
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940803
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 10-10-2018
Publisher: Springer Science and Business Media LLC
Date: 11-2017
Publisher: Springer Berlin Heidelberg
Date: 2013
Publisher: Elsevier BV
Date: 04-2020
Publisher: Elsevier BV
Date: 2015
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 13-11-2013
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 10-2015
Publisher: Elsevier BV
Date: 12-2006
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 06-2017
Publisher: Author(s)
Date: 2017
DOI: 10.1063/1.4991240
Publisher: Hikari, Ltd.
Date: 2014
Publisher: Wiley
Date: 11-1995
Publisher: American Astronomical Society
Date: 17-10-2019
Publisher: Elsevier BV
Date: 02-2011
Publisher: Elsevier BV
Date: 2015
Publisher: Elsevier BV
Date: 2015
Publisher: Elsevier BV
Date: 2015
Publisher: American Astronomical Society
Date: 22-07-2016
Publisher: Elsevier BV
Date: 2015
Publisher: Wiley
Date: 2004
DOI: 10.1002/JGT.20042
Publisher: Pushpa Publishing House
Date: 12-03-2015
Publisher: Elsevier BV
Date: 2015
Publisher: University of Zielona Góra, Poland
Date: 2012
DOI: 10.7151/DMGT.1619
Publisher: Springer Science and Business Media LLC
Date: 16-11-2015
Publisher: Springer Science and Business Media LLC
Date: 11-2017
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940817
Publisher: IOP Publishing
Date: 10-2017
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940815
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940816
Publisher: Elsevier BV
Date: 2015
Publisher: AIP Publishing LLC
Date: 2016
DOI: 10.1063/1.4940811
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 04-2017
Publisher: Informa UK Limited
Date: 08-2018
Publisher: Springer Science and Business Media LLC
Date: 05-06-1998
Publisher: The Institute for Research and Community Services (LPPM) ITB
Date: 07-2013
Publisher: Elsevier BV
Date: 05-2013
Publisher: Elsevier BV
Date: 2015
Publisher: Elsevier BV
Date: 12-2006
Publisher: Elsevier BV
Date: 2015
Publisher: Springer Science and Business Media LLC
Date: 02-2008
Publisher: Elsevier BV
Date: 2008
Publisher: IEEE
Date: 07-2011
Publisher: Elsevier BV
Date: 2015
Publisher: AIP
Date: 2012
DOI: 10.1063/1.4724150
Publisher: Elsevier BV
Date: 2015
No related grants have been discovered for Salvador Duarte Puertas.