ORCID Profile
0000-0001-6384-7450
Current Organisation
The University of Auckland
Does something not look right? The information on this page has been harvested from data sources that may not be up to date. We continue to work with information providers to improve coverage and quality. To report an issue, use the Feedback Form.
Publisher: Cambridge University Press (CUP)
Date: 2018
DOI: 10.1017/PASA.2018.18
Abstract: We present observations of 50 deg 2 of the Mopra carbon monoxide (CO) survey of the Southern Galactic Plane, covering Galactic longitudes l = 300–350° and latitudes | b | ⩽ 0.5°. These data have been taken at 0.6 arcmin spatial resolution and 0.1 km s −1 spectral resolution, providing an unprecedented view of the molecular clouds and gas of the Southern Galactic Plane in the 109–115 GHz J = 1–0 transitions of 12 CO, 13 CO, C 18 O, and C 17 O. We present a series of velocity-integrated maps, spectra, and position-velocity plots that illustrate Galactic arm structures and trace masses on the order of ~10 6 M ⊙ deg −2 , and include a preliminary catalogue of C 18 O clumps located between l = 330–340°. Together with the information about the noise statistics of the survey, these data can be retrieved from the Mopra CO website and the PASA data store.
Publisher: American Astronomical Society
Date: 17-08-2010
Publisher: Oxford University Press (OUP)
Date: 03-2016
DOI: 10.1093/MNRAS/STW191
Publisher: American Astronomical Society
Date: 08-2012
Publisher: American Astronomical Society
Date: 16-08-2011
Publisher: American Astronomical Society
Date: 10-03-2016
Publisher: American Astronomical Society
Date: 07-04-2014
Publisher: Oxford University Press (OUP)
Date: 30-09-2015
Publisher: American Astronomical Society
Date: 11-2013
Publisher: American Astronomical Society
Date: 16-10-2015
Publisher: Oxford University Press (OUP)
Date: 30-01-2014
Publisher: American Astronomical Society
Date: 13-08-2012
Publisher: American Astronomical Society
Date: 27-06-2202
Publisher: American Astronomical Society
Date: 25-11-2015
Publisher: American Astronomical Society
Date: 28-01-2013
Publisher: American Astronomical Society
Date: 20-10-2016
Publisher: American Astronomical Society
Date: 17-12-2013
Publisher: American Astronomical Society
Date: 27-05-2014
Publisher: American Astronomical Society
Date: 28-04-2015
Publisher: Oxford University Press (OUP)
Date: 16-02-2011
Publisher: American Astronomical Society
Date: 07-11-2016
Publisher: American Astronomical Society
Date: 06-07-2012
Publisher: American Astronomical Society
Date: 06-2018
Publisher: American Astronomical Society
Date: 15-12-2016
Publisher: American Astronomical Society
Date: 27-04-2015
Publisher: American Astronomical Society
Date: 31-07-2012
Publisher: EDP Sciences
Date: 12-04-2011
Publisher: American Astronomical Society
Date: 11-09-2015
Publisher: American Astronomical Society
Date: 13-12-2016
Publisher: American Astronomical Society
Date: 07-07-2016
Publisher: IOP Publishing
Date: 25-10-2016
Publisher: American Astronomical Society
Date: 27-01-2014
Publisher: American Astronomical Society
Date: 05-05-2014
Publisher: American Astronomical Society
Date: 11-08-2015
Publisher: American Astronomical Society
Date: 08-01-2015
Publisher: American Astronomical Society
Date: 27-02-2017
Publisher: American Astronomical Society
Date: 12-10-2011
Publisher: American Astronomical Society
Date: 02-03-2016
Publisher: American Astronomical Society
Date: 30-05-2014
Publisher: American Astronomical Society
Date: 22-03-2016
Publisher: American Astronomical Society
Date: 23-04-2013
Publisher: American Astronomical Society
Date: 14-11-2012
Publisher: EDP Sciences
Date: 27-03-2013
Publisher: American Astronomical Society
Date: 27-11-2013
Publisher: American Association for the Advancement of Science (AAAS)
Date: 04-07-2014
Abstract: Many known exoplanets (planets outside our own solar system) are hosted by binary systems that contain two stars. These planets normally circle around both of their stars. Using microlensing data taken with a worldwide network of telescopes, Gould et al. found a planet twice the mass of Earth that circles just one of a pair of stars. The same approach has the potential to uncover other similar star systems and help to illuminate some of the mysteries of planet formation. Science , this issue p. 46
Publisher: American Astronomical Society
Date: 24-09-2014
Publisher: American Astronomical Society
Date: 28-01-2011
Publisher: American Astronomical Society
Date: 22-06-2016
Publisher: American Astronomical Society
Date: 17-01-2013
Publisher: American Astronomical Society
Date: 06-05-2013
Publisher: American Astronomical Society
Date: 26-10-2016
Publisher: American Astronomical Society
Date: 07-09-2030
Publisher: American Astronomical Society
Date: 02-05-2012
Publisher: Oxford University Press (OUP)
Date: 03-04-2013
DOI: 10.1093/MNRAS/STT318
Publisher: Oxford University Press (OUP)
Date: 23-05-2017
Abstract: We present the first catalogue of eclipsing binaries in two MOA (Microlensing Observations in Astrophysics) fields towards the Galactic bulge, in which over 8000 candidates, mostly contact and semidetached binaries of periods & d, were identified. In this paper, the light curves of a small number of interesting candidates, including eccentric binaries, binaries with noteworthy phase modulations and eclipsing RS Canum Venaticorum type stars, are shown as ex les. In addition, we identified three triple object candidates by detecting the light-travel-time effect in their eclipse time variation curves.
Publisher: American Astronomical Society
Date: 23-08-2023
Abstract: The astrometric precision and accuracy of an imaging camera is often limited by geometric optical distortions. These must be calibrated and removed to measure precise proper motions, orbits, and gravitationally lensed positions of interesting astronomical objects. Here, we derive a distortion solution for the OSIRIS Imager fed by the Keck I adaptive optics system at the W. M. Keck Observatory. The distortion solution was derived from images of the dense globular clusters M15 and M92 taken with OSIRIS in 2020 and 2021. The set of 403 starlists, each containing ∼1000 stars, were compared to reference Hubble catalogs to measure the distortion-induced positional differences. OSIRIS was opened and optically realigned in 2020 November and the distortion solutions before and after the opening show slight differences at the ∼20 mas level. We find that the OSIRIS distortion closely matches the designed optical model: large, reaching 20 pixels at the corners, but mostly low order, with the majority of the distortion in the 2nd-order mode. After applying the new distortion correction, we find a median residual of [ x, y ] = [0.052, 0.056] pixels ([0.51, 0.56] mas) for the 2020 solution, and [ x, y ] = [0.081, 0.071] pixels ([0.80, 0.71] mas) for the 2021 solution. Comparison between NIRC2 images and OSIRIS images of the Galactic center show that the mean astrometric difference between the two instruments reduces from 10.7 standard deviations to 1.7 standard deviations when the OSIRIS distortion solution is applied. The distortion model is included in the Keck AO Imaging data-reduction pipeline and is available for use on OSIRIS data.
Publisher: American Astronomical Society
Date: 28-01-2015
Publisher: American Astronomical Society
Date: 03-07-2017
Publisher: American Astronomical Society
Date: 08-01-2013
Publisher: Oxford University Press (OUP)
Date: 09-12-2016
Location: United States of America
No related grants have been discovered for Matthew Freeman.