Astropy: A community Python package for astronomy

Robitaille, Thomas; Tollerud, Erik; Greenfield, P.; Droettboom, Michael; Bray, Erik M.; Aldcroft, T. L.; Davis, M. Ryleigh; Ginsburg, Adam; Price-Whelan, Adrian M.; Kerzendorf, Wolfgang; Conley, A.; Crighton, Neil H. M.; Barbary, Kyle; Muna, Demitri; Ferguson, Henry C.; Grollier, Frédéric; Parikh, Madhura M.; Nair, Prasanth H.; Günther, H. M.; Deil, C.; Woillez, J.; Conseil, Simon; Kramer, Roban Hultman; Turner, James; Singer, L. P.; Fox, R. T.; Weaver, B. A.; Zabalza, V.; Edwards, Zachary; Bostroem, K. A.; Burke, Douglas; Casey, Andrew R.; Crawford, S.; Dencheva, Nadia; Ely, Justin; Jenness, Tim; Labrie, Kathleen; Lim, Pey Lian; Pierfederici, F.; Pontzen, Andrew; Ptak, A.; Refsdal, Brian L.; Servillat, Mathieu; Streicher, O.

doi:10.1051/0004-6361/201322068

Cited by 9,448 publications

(595 citation statements)

References 15 publications

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“…We are grateful to Amelia Bayo for providing us with an electronic version of the Collinder 69 catalog. This research made use of Astropy, a community-developed core Python package for Astronomy (Robitaille et al 2013). This work has made an extensive use of Topcat (http://www.star.bristol.ac.uk/~mbt/topcat/, Taylor 2005).…”

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confidence: 99%

Orion revisited

Bouy

Alves

Bertin

et al. 2014

A&A

119

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Aims. Following the recent discovery of a large population of young stars in front of the Orion nebula, we carried out an observational campaign with the DECam wide-field camera covering ≈10 deg 2 centered on NGC 1980 to confirm, probe the extent of, and characterize this foreground population of pre-main-sequence stars. Methods. We used multiwavelength wide-field images and catalogs to identify potential foreground pre-main-sequence stars using a novel probabilistic technique based on a careful selection of colors and luminosities. Results. We confirm the presence of a large foreground population towards the Orion A cloud. This population contains several distinct subgroups, including NGC 1980 and NGC 1981, and stretches across several degrees in front of the Orion A cloud. By comparing the location of their sequence in various color-magnitude diagrams with other clusters, we found a distance and an age of 380 pc and 5 ∼ 10 Myr, in good agreement with previous estimates. Our final sample includes 2123 candidate members and is complete from below the hydrogen-burning limit to about 0.3 M , where the data start to be limited by saturation. Extrapolating the mass function to the high masses, we estimate a total number of ≈2600 members in the surveyed region. Conclusions. We confirm the presence of a rich, contiguous, and essentially coeval population of about 2600 foreground stars in front of the Orion A cloud, loosely clustered around NGC 1980, NGC 1981, and a new group in the foreground of the OMC-2/3. For the area of the cloud surveyed, this result implies that there are more young stars in the foreground population than young stars inside the cloud. Assuming a normal initial mass function, we estimate that between one to a few supernovae must have exploded in the foreground population in the past few million years, close to the surface of Orion A, which might be responsible, together with stellar winds, for the structure and star formation activity in these clouds. This long-overlooked foreground stellar population is of great significance, calling for a revision of the star formation history in this region of the Galaxy.

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confidence: 99%

Orion revisited

Bouy

Alves

Bertin

et al. 2014

A&A

119

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“…This research has benefitted from the M, L, T, and Y dwarf compendium housed at DwarfArchives.org. This research made use of Astropy, a community-developed core Python package for Astronomy (Robitaille et al 2013 …”

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confidence: 99%

The brown dwarf atmosphere monitoring (BAM) project

Wilson

Rajan

Patience

2014

A&A

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Using the SofI instrument on the 3.5 m New Technology Telescope, we have conducted an extensive near-infrared monitoring survey of an unbiased sample of 69 brown dwarfs spanning the L0 to T8 spectral range, with at least one example of each spectral type. Each target was observed for a 2−4 h period in the J s -band, and the median photometric precision of the data is ∼0.7%. A total of 14 brown dwarfs were identified as variables with min-to-max amplitudes ranging from 1.7% to 10.8% over the observed duration. All variables satisfy a statistical significance threshold with a p-value ≤5% based on comparison with a median reference star light curve. Approximately half of the variables show pure sinusoidal amplitude variations similar to 2MASSJ2139+0220, and the remainder show multi-component variability in their light curves similar to SIMPJ0136+0933. It has been suggested that the L-T transition should be a region of a higher degree of variability if patchy clouds are present, and this survey was designed to test the patchy cloud model with photometric monitoring of both the L-T transition and non-transition brown dwarfs. The measured frequency of variables is 13 +10 −4 % across the L7−T4 spectral range, indistinguishable from the frequency of variables of the earlier spectral types (30 +11 −8 %), the later spectral types (13 +10 −4 %), or the combination of all non-transition region brown dwarfs (22 +7 −5 %). The variables are not concentrated in the transition, in a specific colour, or in binary systems. Of the brown dwarfs previously monitored for variability, only ∼60% maintained the state of variability (variable or constant), with the remaining switching states. The 14 variables include 9 newly identified variables that will provide important systems for follow-up multi-wavelength monitoring to further investigate brown dwarf atmosphere physics.

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“…We load and analyze the HEALPix files in python using healpy and astropy (Robitaille et al 2013). We consider the 99% credible region for GW localization, and hereafter refer to it as a "patch".…”

Section: Discussionmentioning

confidence: 99%

Geographic and Annual Influences on Optical Follow-up of Gravitational Wave Events

Srivastava

Bhalerao

Ravi

et al. 2017

ApJ

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We investigate the effects of observatory locations on the probability of discovering optical/infrared counterparts of gravitational wave sources. We show that for the LIGO-Virgo network, the odds of discovering optical/infrared (OIR) counterparts show some latitude dependence, but weak or no longitudinal dependence. A stronger effect is seen to arise from the timing of LIGO/Virgo observing runs, with northern OIR observatories having better chances of finding the counterparts in northern winters. Assuming identical technical capabilities, the tentative mid-2017 three-detector network observing favors southern OIR observatories for discovery of EM counterparts.

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Astropy: A community Python package for astronomy

Cited by 9,448 publications

References 15 publications

Orion revisited

Orion revisited

The brown dwarf atmosphere monitoring (BAM) project

Geographic and Annual Influences on Optical Follow-up of Gravitational Wave Events

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