Astroquery v0.1

Ginsburg, Adam; Booker, Joseph; Armstrong, Caden; Edward, .; Miller, A. A.; Parejko, John K.; Groener, Austen; Svoboda, Brian; Persson, M. V.; Günther, Hans Moritz; Singer, L. P.; Mirocha, Jordan; Tollerud, Erik; Willett, Kyle; Parikh, Madhura; Droettboom, Michael; Rol, E.; Barbary, Kyle; james-allen,; Séguin-Charbonneau, Loïc; Sipőcz, Brigitta; adamginsburg,; Woillez, J.; Moolekamp, Fred; Shiga, David; Liedtke, Simon; Grollier, Frédéric; Deil, C.; Robitaille, Thomas; Egeland, Ricky

doi:10.6084/m9.figshare.805208.v2

Cited by 11 publications

(8 citation statements)

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“…Software: Astropy (Astropy Collaboration et al 2013), Astroquery (Ginsburg et al 2013), AstroML (VanderPlas et al 2012Ivezić et al 2013), pywcsgrid2 (J. Lee), 8 K2fov (Mullally et al 2016)…”

Section: Gyrochronological Ages For Individual Hyades and Praesepe Starsmentioning

confidence: 99%

K2 Rotation Periods for Low-mass Hyads and a Quantitative Comparison of the Distribution of Slow Rotators in the Hyades and Praesepe

Douglas

Curtis

Agüeros

et al. 2019

ApJ

156

170

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We analyze K2 light curves for 132 low-mass (1 > ∼ M * > ∼ 0.1 M ⊙ ) members of the 600-800 Myrold Hyades cluster and measure rotation periods (P rot ) for 116 of these stars. These include 93 stars with no prior P rot measurement; the total number of Hyads with known P rot is now 232. We then combine literature binary data with Gaia DR2 photometry and astrometry to select single star sequences in the Hyades and its roughly coeval Praesepe open cluster, and derive a new reddening value of A V = 0.035±0.011 for Praesepe. Comparing the effective temperature-P rot distributions for the Hyades and Praesepe, we find that solar-type Hyads rotate, on average, 0.4 d slower than their Praesepe counterparts. This P rot difference indicates that the Hyades is slightly older than Praesepe: we apply a new gyrochronology model tuned with Praesepe and the Sun, and find an age difference between the two clusters of 57 Myr. However, this P rot difference decreases and eventually disappears for lower-mass stars. This provides further evidence for stalling in the rotational evolution of these stars, and highlights the need for more detailed analysis of angular-momentum evolution for stars of different masses and ages.

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Section: Gyrochronological Ages For Individual Hyades and Praesepe Starsmentioning

confidence: 99%

K2 Rotation Periods for Low-mass Hyads and a Quantitative Comparison of the Distribution of Slow Rotators in the Hyades and Praesepe

Douglas

Curtis

Agüeros

et al. 2019

ApJ

156

170

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“…Software: AstroPy (Astropy Collaboration et al 2013), Astroquery (Ginsburg et al 2013), ccdproc (Craig et al 2015), Pythonaliasesandshortcuts (Morgenthaler & Morgenthaler2019),DataThiefIII(Tummers2006),IDL(Harris Geospatial Solutions 2018), IoIO control, reduction, and analysis software (Morgenthaler 2019), matplotlib (Hunter 2007), NumPy (Oliphant 2006), scikit-image (van der Walt et al 2014…”

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Large Volcanic Event on Io Inferred from Jovian Sodium Nebula Brightening

Morgenthaler

Rathbun

Schmidt

et al. 2019

ApJL

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“…The code used to generate the figures in this paper is hosted at https://github.com/rodluger/starrynight. Software: astroquery (Ginsburg et al 2013(Ginsburg et al , 2019, Eigen v3 (Guennebaud et al 2010), exoplanet (Foreman-Mackey et al 2020), pybind11 (Jakob et al 2017, pymc3 (Salvatier et al 2016), scipy (Jones et al 2001), starry (Luger et al 2018), theano (Theano Development Team 2016).…”

Section: Discussionmentioning

confidence: 99%

Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons

Luger,

Agol,

Bartolić

et al. 2021

Preprint

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We derive efficient, closed form, differentiable, and numerically stable solutions for the flux measured from a spherical planet or moon seen in reflected light, either in or out of occultation. Our expressions apply to the computation of scattered light phase curves of exoplanets, secondary eclipse light curves in the optical, or future measurements of planet-moon and planet-planet occultations, as well as to photometry of solar system bodies. We derive our solutions for Lambertian bodies illuminated by a point source, but extend them to model illumination sources of finite angular size and rough surfaces with phase-dependent scattering. Our algorithm is implemented in Python within the open-source starry mapping framework and is designed with efficient gradient-based inference in mind. The algorithm is ∼4 − 5 orders of magnitude faster than direct numerical evaluation methods and ∼10 orders of magnitude more precise. We show how the techniques developed here may one day lead to the construction of two-dimensional maps of terrestrial planet surfaces, potentially enabling the detection of continents and oceans on exoplanets in the habitable zone.

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Astroquery v0.1

Cited by 11 publications

References 0 publications

K2 Rotation Periods for Low-mass Hyads and a Quantitative Comparison of the Distribution of Slow Rotators in the Hyades and Praesepe

K2 Rotation Periods for Low-mass Hyads and a Quantitative Comparison of the Distribution of Slow Rotators in the Hyades and Praesepe

Large Volcanic Event on Io Inferred from Jovian Sodium Nebula Brightening

Analytic Light Curves in Reflected Light: Phase Curves, Occultations, and Non-Lambertian Scattering for Spherical Planets and Moons

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