adsabs/AstroCLIMB huggingface dataset:
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: CCFs of 1.8 m spectra near orbital phases 0.25 and 0.75 from the 1922 (top row) and 1937 (bottom row) campaigns. The spectra have been cross-correlated with the reference spectrum between wavelengths 4300 and 4600 Å using the IRAF task FXCOR. The dominant peak in the CCFs is formed by lines in the spectrum of the primary, while a lower-amplitude peak due to the secondary is marked with a red arrow. The thick red line has a length of 400 km s–1, which is the approximate full amplitude of the radial velocity variation of the primary. The separation between the peaks due to the primary and secondary varies, corresponding to ∼100–190 km s–1, which is smaller than the difference in component velocities found in most other studies. That the radial velocity amplitude of the secondary is smaller than that of the primary is consistent with it being the more massive star. The dashed line is a Gaussian fit to the peak from the primary. The width of the peak in the CCFs formed by the primary near phase 0.25 is greater than that near phase 0.75, and this is also seen in the CCFs of the 1.2 m spectra in Figure 14.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Same as Figure 13, but showing CCFs constructed from 1.2 m spectra. The peak due to the secondary is less well defined than in Figure 13, reflecting the lower S/N of the 1.2 m spectra. Still, the velocity amplitude based on these CCFs is consistent with that obtained from the 1922 campaign spectra. As in Figure 13, the peaks are broader near phase 0.25 than near phase 0.75. As the 1.2 m spectra were recorded with an image slicer, then it is unlikely that this broadening is a consequence of seeing variations.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Comparisons with synthetic spectra. The spectra of PS are the means of many of the 1.8 m spectra recorded between 1922 and 1938 that fall within each phase interval. Spectra 7302 and 7006 were excluded because of poor S/Ns (see text), as were spectra 26304 and 26329 from the 1937 campaign. Hγ in the synthetic spectrum is consistently deeper than that observed. There is better agreement with He I λ4471 at phases 0.2–0.3 and 0.7–0.8. The models consistently underestimate the depth of He I λ4388. A comparison of the synthetic and observed line profiles near phases 0.25 and 0.75, including the location of the notch produced by the secondary in the profile, suggests that the overall contribution of the secondary to the total light from the system is more or less reproduced in the synthetic spectrum. However, that the synthetic spectra are broader than the upper portions of Hγ and He I λ4471 near phases 0.25 and 0.75 is consistent with the orbital velocity of the secondary having been overestimated.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Comparing campaign and synthetic spectra. The spectra of PS are the means of the 1.8 m spectra from the 1922 (top panel) and 1937 campaigns (bottom row). The phase interval 0.7–0.8 is not included because there is only one usable spectrum that samples this interval in the 1922 data set. Hγ is consistently larger in the synthetic spectra than in either group of campaign spectra, with the difference being greatest for the 1937 spectra between phases 0.2 and 0.3. In contrast, the depth of He I λ4471 is more or less reproduced by the models. It is argued in the text that the comparatively shallow nature of Hγ near phase 0.25 in the 1937 spectrum was a transient phenomenon.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Radial velocities measured from digitized 1.8 m spectra using different techniques. The top panel shows CCF-based velocities, while the lower panel shows velocities of the primary estimated from the cores of Hγ and He I λ4471. The red crosses in both panels are the velocities measured by J. S. Plaskett (1922) from a number of lines and summarized in his “Table of Velocities and Residuals.” The solid and dashed curves are the radial velocity curves based on the orbital elements calculated by N. Linder et al. (2008).
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: The model we generated for the stellar spectrum provides a sufficient match to the observed spectrum over the G141 wavelength range for use in our wavelength calibration.
Paper: Old Dogs, New Tricks: Re-examining Photographic Spectra of Plaskett’s Star
Authors: T. J. Davidge
Figure caption: Spectra from the 1922 campaign that sample orbital phases near 0.25 and 0.75 are compared with the CCF template, shown in green. The template consists of unbroadened lines that correspond to H, He, and N transitions, with depths based on those of the actual lines in the median 1922 campaign spectrum. The dotted lines mark the boundaries of the wavelength interval used to generate the CCFs.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: Visualization of white-light light-curve fit for the highest-weighted systematic model for L 98-59 c, which demonstrates a good model fit to the observed data. Panel (a) shows the band-integrated light curve. Panel (b) shows the detrended light curve as well as the best-fitting transit model. The instrumental effects and transit model parameters were fit for simultaneously. Panel (c) shows the residuals between the data and the best-fitting model.
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 getsf-identified filament skeletons are marked over the moment-0 map of 13CO (J = 2–1) emission. The moment-0 map is identical to that in Figure 2(a), and the contour is at the 3σ level. (b) The distribution of Class I YSO candidates is shown in the region bounded by dotted yellow lines, with filled cyan circles outlined in black. (c) Two open blue circles over the moment-0 map indicate the possible extent of Hub-1 and Hub-2. Black arrows indicate small-scale (≲1 pc) filaments within the hubs. Both the hubs are zoomed-in using VVV Ks-band image in the insets. The open red rectangles in the insets indicate the embedded color excess sources with H − Ks > 1.8. The red circular regions over the filament skeletons are utilized to extract the average velocity and velocity dispersion along the filaments, which are shown in Figure 5. The area of the magenta dashed–dotted rectangular region is shown using a two-color composite image in Figure 10(a).
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) Herschel three-color composite image. The colors red, green, and blue present Herschel 500, 350, and 250 μm continuum images, respectively. The plus symbol indicates the position of the 22 GHz H2O and Class I 95 GHz CH3OH maser emissions. The asterisks denote the positions of the ATLASGAL clumps from J. S. Urquhart et al. (2018). Notably, the clumps exhibiting active outflows are marked in black (A. Y. Yang et al. 2022). Panels (b) and (c) display Herschel column density (i.e., N(H2)) and dust temperature (i.e., Td) maps, respectively. The contours in each panel show the SUMSS 843 MHz radio continuum emission. The contour levels are at about [3, 6, 9, 12, and 15] × σ, where 1σ ~ 1 mJy beam−1. In panel (b), arrows highlight high column density regions. Yellow arrows indicate areas characterized by higher dust temperatures and the detection of radio emissions, while cyan arrows denote regions with lower dust temperatures and no detectable radio sources. The rectangular regions highlighted in panel (c) are zoomed-in within the insets. The contours in the top-left and bottom-right insets represent MeerKAT 1.28 GHz radio continuum emission at [5, 15, 30, and 50] × σ and [5, 50, and 160] × σ, respectively, where 1σ ~ 20 μJy beam−1. A gray circle at the bottom-left corner of each inset indicates the beam size (~ 8″ × 8″) of the MeerKAT data. A scale bar of 5 pc is shown in each panel at a distance of 1.98 kpc.
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) SEDIGISM 13CO(J = 2–1) integrated intensity (i.e., the moment-0) map at vlsr of [−38.25, −27.25] km s−1. The contour levels are at [3, 11, 19, 27, 35, and 43] × σ, where 1σ ~ 0.6 K km s−1. The dotted white rectangle indicates the area of Herschel continuum images shown in Figure 1. (b) The peak intensity map for the same molecular line data. (c) The intensity-weighted velocity (i.e., the moment-1) map. (d) The velocity distribution corresponding to the peak intensity, referred to here as the “peak velocity map.” The images in panels (b), (c), and (d) are clipped below the 3σ level of the moment-0 map. The asterisks are the same as in Figure 1. A scale bar of 10 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)–(o) present integrated intensity maps of 13CO(J = 2–1) emission (using filled contours) for vlsr starting from −38.25 to −27.25 km s−1 with an interval of about 0.75 km s−1. The contour levels are at [0.1, 0.2, 0.3, 0.4, 0.5, 0.6, 0.8, and 1.0] × peak moment-0 values, which are mentioned in the respective panels. The open black rectangle shown in panel (g) is zoomed-in using the ATLASGAL 870 μm continuum image in Figure 6(a). A scale bar of 10 pc is shown in panel (m).
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) show the average velocities along filaments F1–F7 for the circular regions depicted in Figure 4(c). The velocity dispersion for these regions is shown using the color scale. The red straight lines indicate the best linear fit to the average velocity distributions. The slopes of the best-fit lines for filaments F1, F2, F3, F5, and F6 are provided in their respective panels.
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: The L 98-59 system provides a unique opportunity to probe the cosmic shoreline. In the solar system, the light blue region separates bodies that have atmospheres from those that do not (K. J. Zahnle & D. C. Catling 2017). Gray dots show known rocky exoplanets with R < 1.6 R⊕ and measured masses and radii. The integrated XUV history of L 98-59 is unknown, so the vertical error bars are representative of M dwarfs (E. L. Shkolnik & T. S. Barman 2014).
Paper: The Transmission Spectrum of the Potentially Rocky Planet L 98-59 c
Authors: Thomas Barclay, Kyle B. Sheppard, Natasha Latouf, Avi M. Mandell, Elisa V. Quintana, Emily A. Gilbert, Giuliano Liuzzi, Geronimo L. Villanueva, Giada Arney, Jonathan Brande, Knicole D. Colón, Giovanni Covone, Ian J. M. Crossfield, Mario Damiano, Shawn D. Domagal-Goldman, Thomas J. Fauchez, Stefano Fiscale, Francesco Gallo, Christina L. Hedges, Renyu Hu, Edwin S. Kite, Daniel Koll, Ravi K. Kopparapu, Veselin B. Kostov, Laura Kreidberg, Eric D. Lopez, James Mang, Caroline V. Morley, Fergal Mullally, Susan E. Mullally, Daria Pidhorodetska, Joshua E. Schlieder, Laura D. Vega, Allison Youngblood, Sebastian Zieba
Figure caption: Observations of L 98-59 b and c were taken by HST just 12.5 hr apart. There is correlation between the two observations, which could indicate a common systematic. The L 98-59 b data shown here are from Visit 2 of five, and are the data set most correlated with the HST observations of L 98-59 c.
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: Atmospheric retrieval results for WASP-17 b’s dayside emission spectrum. Top left: retrieved model emission spectra from our JWST/NIRISS data using the positive eclipse depth prior (error bars). Four retrieval configurations are shown: POSEIDON with the A. A. A. Piette & N. Madhusudhan (2020) T–P profile (purple); POSEIDON with the N. Madhusudhan & S. Seager (2009) T–P profile (orange); TauREx with the BD T–P profile (blue); and TauREx with the N. Madhusudhan & S. Seager (2009) T–P profile (green). For each retrieval, the median retrieved spectrum (solid lines) and 1σ and 2σ confidence intervals (shaded contours) are overplotted. Absorption features of prominent molecular bands are annotated. Top right: corresponding retrieved T–P profiles. Middle histograms: posterior probability distributions for several molecules with strong opacity in the NIRISS wavelength range. Lower half: same retrievals for the JWST/NIRISS data with the negative eclipse depth prior. Full quantitative retrieval results are provided in Appendix B, Table B2. A supersolar H2O abundance is favored across all eight retrievals, irrespective of the eclipse depth prior, T–P profile parameterization, and for both retrieval codes.
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: out-of-transit median frame of the NIRISS SOSS CLEAR exposure from transitspectroscopy reduction. The positions of the traces for order 1 in blue and order 2 in red are shown along with the 15 pixel radius extraction aperture. Middle: the same out-of-transit median frame of the NIRISS SOSS CLEAR exposure but now corrected for the zodiacal background. Bottom: median frame of the NIRISS SOSS F277W exposure. Order 0 contaminants corrected in our analysis are framed. Around pixel 750 we can distinguish three field star contaminants impacting order 1.
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: white light curves for order 1 (left) and order 2 (right) with the corresponding best-fit eclipse model (black line for positive eclipse depth prior and pink dotted for negative eclipse depth prior) from the transitspectroscopy reduction using juliet. White data points represent binned observations over time for visualization. Middle: eclipse model-subtracted light-curve residuals, and Gaussian process (GP) model (light gray). The rms scatter of the residuals is indicated for each panel. Bottom: Allan variance plots for the transitspectroscopy reduction with variations of the white light curves with longer bin timescales.
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: WASP-17 b NIRISS SOSS emission spectra obtained using transitspectroscopy (orange), supreme-SPOON (green), and Ahsoka (blue). We represent both positive (orange) and negative (purple) eclipse depth fitting results from the transitspectroscopy reduction. White data points represent actual eclipse depths constrained to negative values. Bottom: brightness temperature of WASP-17 b as a function of wavelength for the three reductions. For values consistent with zero, we represent the 2σ upper limit (downward arrow) computed using the confidence interval.
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: WASP-17 b NIRISS SOSS emission spectra obtained using the transitspectroscopy data reduction and fitted using juliet. NIRISS SOSS order 1 (red) and order 2 (blue) emission spectra from the four pixel bins (light) and at R ~ 100 (solid). The spectral results allowing for negative eclipse depth fitting are shown in purple for both orders.
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: Extracted 2D stellar spectra for order 1 (red) and order 2 (blue) from the transitspectroscopy reduction. We overplot each spectrum for each integration. The order 0 contamination-corrected order 1 stellar spectra are in green. We can see that the feature around 2 μm caused by the contaminant at ~750 x-pixel (see Figure 1 bottom) has been corrected in the green spectra.
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: individual frame of the NIRISS SOSS CLEAR exposure corrected for the zodiacal background from the transitspectroscopy reduction. Bottom: same individual frame with the out-of-transit median frame subtracted. The residuals enable us to identify the 1/f noise banding. We use the out-of-transit median frame to correct each individual frame.
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 mean per-pixel values of absolute magnitude Mr, metallicity [Fe/H], and interstellar dust extinction along the line of sight in the r band, Ar, for a TRILEGAL-simulated sample of 280,000 main-sequence and red giants stars with r < 26, u < 27, 340° < R.A. < 350°, and −1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3 < δ < 1﹩\mathop{.}\limits^{\unicode{x000b0}}﹩3 (a small patch from the SDSS Stripe 82 region) in the u vs. g − i color–magnitude diagram. The mean values are color coded according to the legend below each panel. Contours visualize the sample distribution in each diagram. The strong variation of Mr with the g − i color is seen in the left panel, except for the small patch with u < 16.5 and 1.0 < g − i < 1.5 where red giant stars dominate. The diagonal iso-metallicity boundaries in the middle panel closely correspond to distance (in the range from about 1 kpc to about 100 kpc in the lower left corner). The values of dust extinction, shown in the right panel, are not large (<0.2) because the selected field is at high Galactic latitudes (centered on b = −52°).