adsabs/AstroCLIMB huggingface dataset:
Paper: G321.93-0.01: A Rare Site of Multiple Hub-filament Systems with Evidence of Collision and Merging of Filaments
Authors: A. K. Maity, L. K. Dewangan, N. K. Bhadari, Y. Fukui, A. Haj Ismail, O. R. Jadhav, Saurabh Sharma, H. Sano
Figure caption: (a) The Galactic longitude–velocity (i.e., l–v) diagram for 13CO(J = 2–1) data. The contour is at 10σ, where 1σ ~ 0.016 K deg. The integration range for the Galactic latitude is [−0.41, 0.37] deg. The yellow-dotted line separates two velocity components at about −35.25 km s−1. The peak velocities for the blue- and redshifted components are shown with cyan and magenta dotted lines, respectively. (b) The spatial distribution of the blue- and redshifted components. The blue- and redshifted components are integrated for the velocity ranges [−38.25, −35.50] and [−35.25, −27.25] km s−1, respectively. The contour levels for the blue- and redshifted components are at [3σ, 6σ, 9σ] and [6σ, 15σ, 30σ], respectively. The 1σ values are 0.3 and 0.5 K km s−1 for integrated intensity maps of the blue- and redshifted components, respectively. The areas bounded by the yellow lines are considered for calculating the total mass of the blueshifted component. The PV diagrams are extracted along the arrows highlighted in panel (b), which are shown in Figure 9. (c) Same as panel (b), with redshifted component shifted by about 4.2 pc. The dashed–dotted and solid white rectangles present the initial and final positions of the redshifted cloud component, respectively.
Paper: G321.93-0.01: A Rare Site of Multiple Hub-filament Systems with Evidence of Collision and Merging of Filaments
Authors: A. K. Maity, L. K. Dewangan, N. K. Bhadari, Y. Fukui, A. Haj Ismail, O. R. Jadhav, Saurabh Sharma, H. Sano
Figure caption:                         (a) The two-color composite image presents the 13CO(J = 2–1) integrated intensity maps shown in Figures 3(i) (in cyan) and (k) (in red) for the region highlighted by the dashed–dotted rectangle in Figure 4(c). The moment-0 maps in cyan and red are displayed on a linear scale from 3σ to 18σ and 3σ to 10σ, respectively, where σ ~ 0.15 K km s−1. The open black circle, indicated by a yellow arrow, is Hub-2 as shown in Figure 4(c). The dashed–dotted lines trace the filaments (i.e., F4, F5, and F6) connected to Hub-2. (b) Similar two-color composite image showing 13CO(J = 2–1) integrated intensity maps displayed in Figures 3(i) (in cyan) and (m) (in red) for the area covered by the dashed–dotted polygon in Figure 6(a). The moment-0 maps in cyan and red are displayed on a linear scale from 6σ to 15σ and 3σ to 7σ, respectively. The black circle, situated at the peak emission of ATL-2 (indicated by a yellow arrow), has a radius equal to the leaf's effective radius. The dashed–dotted lines indicate the filaments connected to Leaf-2. A scale bar of 5 pc is shown in each panel.
Paper: G321.93-0.01: A Rare Site of Multiple Hub-filament Systems with Evidence of Collision and Merging of Filaments
Authors: A. K. Maity, L. K. Dewangan, N. K. Bhadari, Y. Fukui, A. Haj Ismail, O. R. Jadhav, Saurabh Sharma, H. Sano
Figure caption: Panels (a)–(g) present the PV diagrams along the arrows A1–A7, as indicated in Figure 8(b). The contour values range from 1 to 10 K, with intervals of 1 K. The red and cyan arrows in each panel indicate two separate velocity components mixed together. The white arrows for A7 point to a single velocity component.
Paper: G321.93-0.01: A Rare Site of Multiple Hub-filament Systems with Evidence of Collision and Merging of Filaments
Authors: A. K. Maity, L. K. Dewangan, N. K. Bhadari, Y. Fukui, A. Haj Ismail, O. R. Jadhav, Saurabh Sharma, H. Sano
Figure caption: (a) The optical depth (i.e., τ13) map. The minimum (Min), maximum (Max), mean, and standard deviation (Std) values for the τ13 map are provided in the panel. (b) The column density (i.e., N(H2)) map for Tex = 15 K. The Min, Max, mean, and Std values for the N(H2) map are indicated in the panel in units of 1021 cm−2. In both panels, the red contour indicates the extent of the 13CO(J = 2–1) emission above the 3σ limit, as shown in Figure 2. A scale bar of 10 pc is displayed in each panel.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: Phase-folded radial velocities from PFS (golden diamonds) and HARPS (purple stars and blue triangles) only, with residuals plotted below.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: Evolutionary track and present evolutionary stage of TOI-4994 based on the best-fit MIST model. The blue line is the MIST track and the black contours represent the 1σ and 2σ constraints on the current temperature and surface gravity from the MIST isochrone, while the green contours show the 1σ and 2σ constraints on Teff and logg* from the EXOFASTv2 fit and observations of the system. The red cross indicates the median value and confidence intervals.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: Light curves of TOI-4994 from the LCOGT and ASTEP-Antarctica ground-based observatories.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: TESS light curves of TOI-4994 at 30 (top), 10 (middle), and 2 (bottom) minute cadences, combining six different sectors. The red lines show the best-fit EXOFASTv2 models, phase-folded on the orbital period.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: RV measurements of TOI-4994 (top) phase-folded on the orbital period (bottom). The black lines show the best-fit EXOFASTv2 models, with the residuals shown below the RV curves.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: Time-series photometry of all six TESS sectors used in our analysis.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: I band speckle image and sensitivity curve for TOI-4994 from the SOAR telescope.
Paper: Discovery and Characterization of an Eccentric, Warm Saturn Transiting the Solar Analog TOI-4994 
Authors: Romy Rodríguez Martínez, Jason D. Eastman, Karen A. Collins, Joseph E. Rodriguez, David Charbonneau, Samuel N. Quinn, David W. Latham, Carl Ziegler, Rafael Brahm, Tyler R. Fairnington, SolÉne Ulmer-Moll, Keivan G. Stassun, Olga Suarez, Tristan Guillot, Melissa J. Hobson, Joshua N. Winn, Shubham Kanodia, Martin Schlecker, R. P. Butler, Jeffrey D. Crane, Steve Shectman, Johanna K. Teske, David Osip, Yuri Beletsky, Matthew P. Battley, Angelica Psaridi, Pedro Figueira, Monika Lendl, François Bouchy, Stéphane Udry, Michelle Kunimoto, Djamel Mékarnia, Lyu Abe, Trifon Trifonov, Marcelo Tala Pinto, Jan Eberhardt, Nestor Espinoza, Thomas Henning, Andrés Jordán, Felipe I. Rojas, Khalid Barkaoui, Howard M. Relles, Gregor Srdoc, Kevin I. Collins, Sara Seager, Avi Shporer, Michael Vezie, Christina Hedges, Ismael Mireles
Figure caption: SED fit for TOI-4994. The horizontal error bars correspond to the bandwidth of each filter, while the error bars in flux are the measurement uncertainties. The black points are the modeled broadband averages.
Paper: JWST-TST DREAMS: A Supersolar Metallicity in WASP-17 b’s Dayside Atmosphere from NIRISS SOSS Eclipse Spectroscopy
Authors: Amélie Gressier, Ryan J. MacDonald, Néstor Espinoza, Hannah R. Wakeford, Nikole K. Lewis, Jayesh Goyal, Dana R. Louie, Michael Radica, Natasha E. Batalha, Douglas Long, Erin M. May, Elijah Mullens, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Lili Alderson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Knicole Colón, Ana Glidden, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Roeland P. van der Marel
Figure caption: Top: atmospheric retrieval results for WASP-17 b’s emission spectra using free chemistry and the BD T–P profile in TauREx. The emission spectra are from the transitspectroscopy data reduction obtained using positive (black) and negative (white) priors for both orders. Bottom: brightness temperatures of WASP-17 b as a function of wavelength for the transitpectroscopy reductions plotted against the best-fit models from the retrieval analysis. Brightness temperatures consistent with zero within the confidence interval are represented as 2σ upper limits.
Paper: JWST-TST DREAMS: A Supersolar Metallicity in WASP-17 b’s Dayside Atmosphere from NIRISS SOSS Eclipse Spectroscopy
Authors: Amélie Gressier, Ryan J. MacDonald, Néstor Espinoza, Hannah R. Wakeford, Nikole K. Lewis, Jayesh Goyal, Dana R. Louie, Michael Radica, Natasha E. Batalha, Douglas Long, Erin M. May, Elijah Mullens, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Lili Alderson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Knicole Colón, Ana Glidden, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Roeland P. van der Marel
Figure caption: Left: brightness temperature of WASP-17 b as a function of wavelength for the transitpectroscopy reduction plotted against the best-fit models from our forward model and retrieval analysis. We additionally show a 1800 K blackbody (red line) and a simple parametric function assuming a geometric albedo of 0.2 (blue line). Right: associated pressure–temperature (P–T) profiles for each of the best-fit models. The red line indicates a 1800 K blackbody temperature.
Paper: JWST-TST DREAMS: A Supersolar Metallicity in WASP-17 b’s Dayside Atmosphere from NIRISS SOSS Eclipse Spectroscopy
Authors: Amélie Gressier, Ryan J. MacDonald, Néstor Espinoza, Hannah R. Wakeford, Nikole K. Lewis, Jayesh Goyal, Dana R. Louie, Michael Radica, Natasha E. Batalha, Douglas Long, Erin M. May, Elijah Mullens, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Lili Alderson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Knicole Colón, Ana Glidden, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Roeland P. van der Marel
Figure caption: Retrieved oxygen-to-hydrogen ratio of WASP-17 b’s dayside atmosphere. Left: O/H constraints using the positive eclipse depth fitting method. Right: O/H constraints using the eclipse depth fitting method allowing negative depths. The O/H ratio posteriors are derived from the full set of posterior samples from each of the eight retrievals shown in Figure 7. The 2σ lower limits for WASP-17 b’s dayside O/H ratio (>6.6 × solar for the positive eclipse depth prior and >1.8 ×​​​​​​ solar for the prior allowing negative eclipse depths) are overplotted for reference (dashed lines).
Paper: JWST-TST DREAMS: A Supersolar Metallicity in WASP-17 b’s Dayside Atmosphere from NIRISS SOSS Eclipse Spectroscopy
Authors: Amélie Gressier, Ryan J. MacDonald, Néstor Espinoza, Hannah R. Wakeford, Nikole K. Lewis, Jayesh Goyal, Dana R. Louie, Michael Radica, Natasha E. Batalha, Douglas Long, Erin M. May, Elijah Mullens, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Lili Alderson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Knicole Colón, Ana Glidden, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Roeland P. van der Marel
Figure caption: Residuals between reductions. White data points correspond to negative eclipse depth values.
Paper: JWST-TST DREAMS: A Supersolar Metallicity in WASP-17 b’s Dayside Atmosphere from NIRISS SOSS Eclipse Spectroscopy
Authors: Amélie Gressier, Ryan J. MacDonald, Néstor Espinoza, Hannah R. Wakeford, Nikole K. Lewis, Jayesh Goyal, Dana R. Louie, Michael Radica, Natasha E. Batalha, Douglas Long, Erin M. May, Elijah Mullens, Sara Seager, Kevin B. Stevenson, Jeff A. Valenti, Lili Alderson, Natalie H. Allen, Caleb I. Cañas, Ryan C. Challener, Knicole Colón, Ana Glidden, David Grant, Jingcheng Huang, Zifan Lin, Daniel Valentine, C. Matt Mountain, Laurent Pueyo, Marshall D. Perrin, Roeland P. van der Marel
Figure caption: Contribution functions corresponding to the best-fitting TauREx model emission spectrum using the N. Madhusudhan & S. Seager (2009) T–P profile and the observed emission spectrum obtained with the positive eclipse depth fitting method. Left: spectral contributions (color scale) showing the pressure range probed by our NIRISS observations at each wavelength. Right: integrated average pressure contribution function.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: The left panel shows SDSS-based empirical absolute magnitude vs. color parameterization for main-sequence stars and red giants. The data are color coded by metallicity, ranging from [Fe/H] = −2.5 to 0 (blue to red). The three lines correspond to three values of metallicity: [Fe/H] = −2, −1, and 0 (dotted–dashed, solid, and dashed, respectively). The middle panel shows a sample of 63,000 stars that have a signal-to-noise ratio for Gaia's parallax measurements of at least 20 (WDs can be seen in the lower left corner). Their absolute magnitudes are derived from parallax measurements. The dotted–dashed, solid, and dashed black lines are the same as in the left panel. For comparison, the essentially identical yellow dotted lines were computed using Equations (A2) and (A7) from Ž. Ivezić et al. (2008). Note the discrepancy between these parameterizations and data for subgiant stars (Mr ~ 3−4 and g − i ~ 0.8−1.1). The right panel shows a sample of 415,000 stars with r < 22 and u < 22 as red dots (shown by blue dots in Figure 1), and 409,000 of those that also have 0.2 < g − i < 3.5 as cyan dots. Their absolute magnitudes were computed using the so-called “photogeometric” distances from C. A. L. Bailer-Jones et al. (2021). The dotted–dashed, solid, and dashed black lines are the same as in the left and middle panels. About 10,000 stars below the main sequence (about 2.5% of the full sample) seen at g − i = 0.4 and Mr > 7 are predominantly found at the faint end (r > 20) and may be outliers due to the low photometric signal-to-noise ratio.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: An illustration of multiple stellar populations. The left panel is a color–magnitude diagram for 841,000 stars from the SDSS Stripe 82 Standard Star Catalog (variable sources are excluded; K. Thanjavur et al. 2021) that have Gaia matches within 0﹩\mathop{.}\limits^{\unicode{x02033}}﹩15 (after correcting for proper motion using Gaia measurements). A subset of 415,000 stars with r < 22 and u < 22 are overplotted as blue dots, and 409,000 of those that also have 0.2 < g − i < 3.5 (dominated by main-sequence stars and red giants) are overplotted as cyan dots. Finally, 63,000 stars that have a signal-to-noise ratio for Gaia's parallax measurements of at least 20 are shown as green dots (these stars can be used for the calibration of luminosity–color relations). The same symbol color scheme is used in the other two panels. The three yellow lines in the middle panel show the stellar locus parameterization used by G. M. Green et al. (2014) for three values of metallicity (left to right): [Fe/H] = −2, −1, and 0. In the right panel, the impact of metallicity on the color–color tracks is negligible and all three are indistinguishable from each other. In the bottom of the middle panel, at −0.5 < g − r < 0, the three dark blue sequences correspond to (from left to right) He WDs, H WDs, and BHB stars. The clouds of pale blue dots visible above the main stellar locus in the middle and right panels correspond to unresolved binary stars (G. R. Smolčić et al. 2004).
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Augmented SDSS color tracks for two isochrone ages (left: 1 Gyr; right: 10 Gyr) and the full metallicity range (−2.5 < [Fe/H] < +0.5, color coded linearly from blue to red). The black dots show the same sample of 63,000 stars from the middle panel in Figure 2. As can be seen in the top right panel, subgiant stars that could not be fit with empirical SDSS-based tracks (see the middle panel in Figure 2) can be explained with tracks for old stars and intermediate-range metallicity. The sharp feature protruding from the main locus in the middle two panels corresponds to most luminous and evolved high-metallicity stars. Note that diagrams in the bottom row, which do not include the u band, show very little dependence on metallicity.
Paper: PhotoD with LSST: Stellar Photometric Distances Out to the Edge of the Galaxy
Authors: Lovro Palaversa, Željko Ivezić, Neven Caplar, Karlo Mrakovčić, Bob Abel, Oleksandra Razim, Filip Matković, Connor Yablonski, Toni Šarić, Tomislav Jurkić, Sandro Campos, Melissa DeLucchi, Derek Jones, Konstantin Malanchev, Alex I. Malz, Sean McGuire, Mario Jurić
Figure caption: Analysis of color degeneracies between giants and main-sequence stars. The left panel shows minimum color distance in four-dimensional color space (u − g, g − r, r − i, and i − z) between a position on the locus with Mr < 4 (giants) and any position on the main-sequence Mr > 4 locus (in magnitudes). Symbols are color coded by metallicity, linearly from blue to red for the range −2.5 to 0.5. The middle and right panels show errors in absolute magnitude and metallicity when a giant is misidentified as a main-sequence star closest to it in color space.