adsabs/AstroCLIMB huggingface dataset:
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: Monte Carlo Analysis 1: can random sampling from an underlying uniform distribution of host-star [Fe/H] produce the observed results? (a) A histogram of the uniform sample. The blue histograms are the distributions of median differences for (b) HJs and CJs, (c) HJs and CCJs, and (d) CEJs and CCJs. The vertical black solid lines in all these figures represent the observed median differences. The region right to this black solid line is colored yellow, where here the median difference ≥ the observed median difference. The probability of median difference ≥ observed median difference is the area under the histogram in the yellow shaded region divided by the total number of counts.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: (a) [Fe/H] distributions of HJ, CEJ, and CCJ hosts. The black curved lines are the KDEs from the colored histograms. The median [Fe/H] distributions of HJs and CEJs are similar, while the CCJ hosts have a lower median [Fe/H]. We also note that for HJ hosts, the [Fe/H] distribution has a longer tail toward high [Fe/H], and CCJs have a long tail toward low metallicity. Also, the [Fe/H] distribution for the CCJs is much flatter. (b) Violin plots showing the [Fe/H] distributions of HJ, CCJ, and CEJ hosts. CCJs and CEJs are denoted by green and red, respectively. (c) Cumulative distributions of [Fe/H] for HJs, CEJs, and CCJs. We can see that the central part of the host-star [Fe/H] distributions of HJs and CEJs resemble each other.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: Host-star [Fe/H] for high- and low-eccentricity planets among HJs, WJs, and CJs. For each group, the low-eccentricity, or “circular,” subgroup is shown on the left, and the eccentric subgroup is shown on the right. HJs are not subdivided into two subgroups due to the lack of eccentric HJs in our sample. We note that, only for CJs, the difference of the median host-star [Fe/H] between the eccentric and circular subgroups is greater than 0.1 dex.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: Comparison of the calibrated Gaia [Fe/H] with (a) GALAH and (b) LAMOST metallicities. The blue points represent the [Fe/H] values of stars common to each pair of instruments. The black solid line is a fitted straight line. The median of the difference (MED) of [Fe/H] values between (a) Gaia and GALAH and (b) Gaia and LAMOST, i.e., the median of (y − x) coordinates of the blue points is shown. The median absolute deviation (MAD) of [Fe/H] differences is also shown.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Surface gravity vs. effective temperature displayed logarithmically for TIC 365102760 along with the other planets discovered by the TESS GTG program (stars) compared to all known planets with well-characterized radii and masses (points). GTG discoveries have almost doubled the number of known systems on the subgiant and red giant branch. Hot Neptunes (3 R⊕ < R  p  < 8 R ⊕, P orb < 10 days) have been highlighted in orange. We also illustrate the MIST evolutionary tracks of 1–2 M ⊙, +0.25 [Fe/H] dex stars in 0.1 M ⊙ increments for reference. We have highlighted a MIST evolutionary track for a 1.4 M ⊙, [Fe/H] = 0.25 dex star in red, illustrating the rough evolutionary sequence probed by the GTG survey.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Full TESS prime mission light curves of TIC 365102760, produced using the Quick Look Pipeline (QLP) KSPSAP detrending, the QLP SAP detrending, the eleanor pipeline, and the giants pipeline, from top to second from bottom. Additional data have since been acquired by the TESS extended mission at higher cadence for TIC 365102760 and converted into a light curve via the SPOC pipeline, plotted in the bottom row. The scatter is noticeably higher for the high-cadence light curve.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: Velocity dispersion (left column) and age distributions (right column) of the HJ, WJ, CEJ, and CCJ hosts. The distributions are obtained using the bootstrapped resampling method described in the text. We find that HJ hosts are younger with the smallest velocity dispersion.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Phase-folded light curves showing phase vs. normalized flux of TIC 365102760 using the QLP “KSPSAP FLUX,” “SAP FLUX,” eleanor, giants, and SPOC pipelines (from top to bottom, respectively). Clear differences in transit depth and shape and light-curve scatter can be seen between the different light curves. The SPOC data cover a shorter baseline (only 27 days) but have a 15 times higher cadence than the other light curves.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Periodogram of the Keck/HIRES RV measurements of TIC 365102760. The strongest signal present in the data, which does not correspond to a known alias of the Earth or Moon, is highlighted with a blue point. We find a power excess in the RV measurements at 4.2 days, with a ΔBIC = 25.5, just below the false-alarm probability threshold of ΔBIC = 33 found to validate a planetary signal without additional information. This signal matches the period and phase of the signal found in the light curve of TIC 365102760.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: BLS power as a function of period for the five light curves of TIC 365102760 shown in Figure 1. The period of highest power has been highlighted with a black dashed line and its harmonics with gray dashed lines. The 4.2 days transit signal is only visible in the giants and SPOC light curves, while going undetected in the others.
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption: Possible distribution of ﹩\mathrm{log}{Q}_{* }^{{\prime} }﹩. Here we assume the inspiral timescale is ∼6 Gyr and the HJs that have been destroyed had similar planetary and stellar properties. The median and 16th and 84th percentiles are ﹩\mathrm{log}{Q}_{* }^{{\prime} }\approx 6\pm 1.﹩
Paper: Host-star Properties of Hot, Warm, and Cold Jupiters in the Solar Neighborhood from Gaia Data Release 3: Clues to Formation Pathways
Authors: Bihan Banerjee, Mayank Narang, P. Manoj, Thomas Henning, Himanshu Tyagi, Arun Surya, Prasanta K. Nayak, Mihir Tripathi
Figure caption:  T eff distributions of the host stars of HJs, WJs, CEJs, and CCJs. In terms of T eff we do not see a significant difference.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Planet radius vs. the fraction of estimated total atmospheric mass loss divided by the current planet mass for all planets with masses and radii reported with ≥50% accuracy, with ages from the NASA Exoplanet Archive accessed on 2023 January 31. The color indicates the atmospheric mass-loss rate in grams per second. Evolved planets have been highlighted with stars, where TIC 365102760 b is indicated by the largest star. The average errors are illustrated in the upper right-hand corner of the figure. TIC 365102760 b both has a higher current mass-loss rate and is predicted to have experienced more atmospheric mass loss than all other gaseous planets, with only a few rocky planets experiencing higher rates of mass loss. As the atmospheric mass for this planet is predicted to be smaller than the total mass expected to have been lost, it is unclear how TIC 365102760 b has retained an atmosphere given its current radius and orbit around its host star.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Semimajor axis divided by stellar radius vs. planet-to-star mass ratio for confirmed planets. The orbital decay timescales are determined assuming a tidal decrease toward the upper left of this plot, where the black diagonals correspond to theorized rates of orbital decay, with the leftmost line corresponding to a decay timescale of 106 yr and each following line increasing by a factor of 10. The blue points have stellar effective temperatures <6000 K, as reported by the NASA Exoplanet Archive, while the red points represent planets around hotter stars. The planets confirmed by our second TESS GTG paper (Grunblatt et al. 2022) are shown as squares with black outlines and are populating relatively sparse regions of parameter space on this plot that correspond to rapid orbital decay. TIC 365102760 b may be experiencing the fastest rate of orbital decay of any planetary system known with a mass ratio below 10−4 or a planet mass <25 M ⊕.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Planet radius vs. age for two toy models of TIC 365102760 b that agree with the median mass, radius, age, and flux measured here (black points). A planet model following the rapid reinflation formulation of Thorngren et al. (2021) is shown in blue, while an atmospheric mass-loss model following the formulation of Thorngren et al. (2023), tuned such that we recover the measured planet mass and radius at the current system age, is shown in orange. This rapid reinflation model implies the planet was smaller during the main-sequence phase, resulting in a ∼40% reduction in total atmospheric mass loss from TIC 365102760 b relative to models that do not allow late-stage inflation.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Top row: XUV luminosity vs. the logarithm of the stellar age in years for 1 M ⊙ (left) and 1.22 M ⊙ (right) stellar models. The XUV luminosity is defined with respect to the bolometric luminosity of the Sun and is only modeled from 20 Myr after star formation to the end of the red giant branch phase of stellar evolution. Middle row: bolometric luminosity for 1 M ⊙ (left) and 1.22 M ⊙ (right) stellar models, also defined with respect to the bolometric luminosity of the Sun. Bottom row: ratio of XUV flux to bolometric flux as a function of age for 1 M ⊙ (left) and 1.22 M ⊙ (right) stellar models.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Corner plot illustrating the convergence of the stellar parameters determined for TIC 365102760 by fitting the Gaia DR2 G, 2MASS J, H, and K, and WISE W1, W2, and W3 photometry as well as Gaia parallax to MIST isochrones. The stellar mass, radius, and age determined here are independently confirmed via a spectroscopic approach and are shown to agree with isoclassify-determined values within uncertainties.
Paper: TESS Giants Transiting Giants. IV. A Low-density Hot Neptune Orbiting a Red Giant Star
Authors: Samuel K. Grunblatt, Nicholas Saunders, Daniel Huber, Daniel Thorngren, Shreyas Vissapragada, Stephanie Yoshida, Kevin C. Schlaufman, Steven Giacalone, Mason Macdougall, Ashley Chontos, Emma Turtelboom, Corey Beard, Joseph M. Akana Murphy, Malena Rice, Howard Isaacson, Ruth Angus, Andrew W. Howard
Figure caption: Top: the giants light curve of TIC 365102760 folded at a period of 4.21285367 ± 0.00000074 days. The detrended photometry is shown in black, with the binned photometry plotted in green and the best-fit exoplanet model overplotted in orange, with 90% confidence intervals shaded. Bottom: all RV observations of TIC 365102760 (black) along with the best-fit exoplanet model and 90% confidence interval (orange) folded at the orbital period of the planet. Observations come from the Keck I/HIRES spectrograph on Maunakea.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Three models for SN placement in galaxies, each illustrated by placing 100 model-generated SNe in NGC 4303. From left to right—Model 1: the SNe are randomly placed across the footprint of the MUSE Hα map with equal probability assigned to each pixel. Model 2: the SNe are placed based on a probability distribution that follows the distribution of Hα intensities in the MUSE Hα map. Model 3: the SNe are placed based on a probability distribution that follows the near-IR light in the Spitzer 3.6 μm map and therefore approximately traces the overall distribution of stellar mass.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Figure 1 continued.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: H II regions and recent SNe in NGC4303. As Figure 2 for NGC 4303 but now the white contours show the extent of the nebular region catalogs from Groves et al. (2023) and Santoro et al. (2022).
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Distances to nearest H II region. Left: KDE of the distances from each SN site to the nearest H II region. SNe with distances less than 1 pc are found within an H II region. SNe II are represented with dashed–dotted, dark-purple; SNe Ia with solid red-purple; SESNe with dashed magenta; and unclassifed SNe with dotted peach. Vertical color-and-style-coded lines mark the median distance value for each SN type. Gray shaded region marks the pixel scale. Right: CDFs of the distances to the nearest H II region for our real SN sample and three modeled populations. Our real SNe sample is drawn with a dark-gray line. The randomly generated SNe sample is drawn from the local (500 and 1000 pc) map around each SN site. The 500 pc random pull sample is plotted with a dotted magenta line and the 1000 pc with a dashed peach line. The population generated from the Hα distribution is plotted as a dashed, dark-purple line, and the stellar disk distribution as a dashed–dotted red-purple line. The transparent shading represents the 16th–84th percentile values from 1000 random pulls each the size of our observed SN sample from each model distribution. We find that our SESNe are overwhelmingly located in the line of sight to our H II regions, while our SNe Ia sample tends to be less associated with H II regions, and our SNe II are somewhere in between. Our real SN sample is distributed between our Hα model sample and our stellar disk and random local models.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Comparison of PHANGS–MUSE (left panels) and HST (right panels) Hα emission cutouts (500 × 500 pc) centered on the locations of the SNe in our sample. SNe are marked with green circles. SNe are labeled with their host galaxy and type classification in the title of each subplot row. Each panel is oriented with the top of the figure as north; east is left.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Figure A4 continued.
Paper: Hα Emission and H II Regions at the Locations of Recent Supernovae in Nearby Galaxies
Authors: Ness Mayker Chen, Adam K. Leroy, Sumit K. Sarbadhicary, Laura A. Lopez, Todd A. Thompson, Ashley T. Barnes, Eric Emsellem, Brent Groves, Rupali Chandar, Mélanie Chevance, Ryan Chown, Daniel A. Dale, Oleg V. Egorov, Simon C. O. Glover, Kathryn Grasha, Ralf S. Klessen, Kathryn Kreckel, Jing Li, J. Eduardo Méndez-Delgado, Eric J. Murphy, Debosmita Pathak, Eva Schinnerer, David A. Thilker, Leonardo Úbeda, Thomas G. Williams
Figure caption: Figure A1 continued.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: The WISE W1 and Spitzer IRAC 3.6 filter responses in comparison to two different mid-IR SED’s from Brown et al. (2014). Note that W1 and IRAC 3.6 have nearly identical wavelength coverage where 73% of the W1 flux matches 87% of IRAC 3.6. W1 samples its remaining flux to the blue of IRAC 3.6, and IRAC 3.6 samples its remaining flux redward of 3.8 μm. Passive galaxies have steep SED’s (shown as blue) resulting in blue W1-3.6 colors. Star-forming galaxies have flat SED’s resulting in red W1-3.6 colors (opposite to the traditional expectation for galaxy colors). Both filters encompass the 3.3 μm PAH feature associated with AGB stars.
Paper: The Baryonic Tully–Fisher Relation. I. WISE/Spitzer Photometry
Authors: Francis Duey, James Schombert, Stacy McGaugh, Federico Lelli
Figure caption: A comparison between the Dale et al. (2007) IRAC 3.6 photometry of the SINGS sample with the SPARC pipeline. There were 12 galaxies in common, the Dale et al. 3.6 μm magnitudes are shown in comparison with SPARC isophotal magnitudes (measured inside an elliptical aperture defined by the 23 3.6 mag arcsec−2 isophote) and the asymptotic magnitude determined from curves of growth. The blue line represents unity between the magnitude systems, the correspondence is excellent. The residuals are shown in the bottom panels with a normalized histogram for each panel to the far right.