adsabs/AstroCLIMB huggingface dataset:
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Spectroscopic evolution of Nova LMCN 2009-05a during the nebular phase, from day 173 (2009 October 25) to day 261 (2010 January 21). The spectra prominently display strong forbidden lines, including [O III] at 4363, 4959, and 5007 Å, and [N II] at 5755 Å.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: NIR color of LMCN 2009-05a from day 11 to 650 generated using SMARTS.
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Observed optical spectrum (black) of Nova LMCN 2009-05a on 2009 December 27 (day 236), plotted over with the best-fitting CLOUDY model (red).
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Observed optical spectrum (black) of Nova LMCN 2009-05a on 2009 July 23 (day 79), plotted over with the best-fitting CLOUDY model (red).
Paper: The Unexplored Dusty Nova LMCN 2009-05a in the Large Magellanic Cloud
Authors: Mohit Singh Bisht, A. Raj, F. M. Walter, Anatoly S. Miroshnichenko, D. Bisht, K. Belwal, Shraddha Biswas
Figure caption: Spectroscopic evolution of Nova LMCN 2009-05a during the dust formation phase, from day 82 (2009 July 26) to day 171 (2009 October 23). Identified lines are marked, and the time since discovery (in days) is labeled beside each spectrum.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: We compare the F444W photometry and F356W – F444W color of each detected point source (labeled purple icons) to the predicted photometry of stellar and substellar objects modeled at the age and distance of each target star (aka “isochrone curve,” shown in the solid line) in order to rule out background contaminants. The point sources detected in both filters (purple circles) are far removed from the isochrones and thus unlikely to be associated with the target system, however the two F356W dropout sources (purple triangles at the 3σ color limit, and vertical bars at the 1σ color limit) are consistent both with substellar field objects and in the limit of their colors, with a sub-Saturn-mass companion. The color of the marker on the isochrone curve corresponds to the object mass, and the predicted photometry is based on the Ames-COND (circle markers, for M > 0.075 M⊙), ATMO-CEQ (square markers, for 0.075 M⊙ > M > 2 MJup), and BEX-petitCODE (for M ≤ 2 MJup) with the extrapolation to very low masses denoted by the hatched background. For comparison, we show isochrone curves for field age (1 Gyr) populations at 100 pc and 1000 pc in the dashed and dotted lines, respectively.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Color–magnitude diagram of the two dropout candidates (in purple) as compared to the sources in the JADES GOODS-S deep field catalog (in black), demonstrating the rarity of extragalactic sources with F444W magnitude < 24 and F356W – F444W > 1. We show the 3σ and 1σ color limits of the dropout candidates with triangles and vertical bars, respectively. 2M J0944 P1 has the strongest color limit and a correspondingly low likelihood of being a background galaxy.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Data and PSF fit results for the marginally detected “F356W dropout” sources. The first column on the left shows the F356W data, the second column shows the F444W data, the third column shows the best-fit PSF in F444W (using the LSQ fit for HIP 17605 P1 and the spaceKLIP fit for 2M J0944 P1), and the right column shows the residuals in F444W. The PSF fit SNR of HIP 17695 P1 in F444W is 1.64, leading it to be less compelling as an exoplanet candidate. 2M J0944 P1 is detected with an SNR of 3.91, and remains as a marginal detection. As the SNRE of each signal in F356W falls below the threshold of three, we do not perform a PSF model fit for the data in that filter. We note that the positive blob visible in the F356W data for 2M J0944 P1 is offset by several pixels from the location of the source in F444W, and that it has an amplitude similar to the F444W residuals.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Flux maps of all targets in GTO 1184, in the F444W filter. All observations were reduced with RDI using the full library of reference PSFs. Point-like and extended sources are labeled in the images (with names beginning with “P” and “E,” respectively), and the point-like sources are magnified in the image insets. Extended background sources are abundant in the survey, and the edge-on disk of AU Mic is clearly detected.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: Flux maps of all targets in GTO 1184, in the F356W filter. All observations were reduced with RDI using the full library of reference PSFs. Point-like and extended sources are labeled in the images (with names beginning with “P” and “E,” respectively), and the point-like sources are magnified in the image insets. Extended background sources are abundant in the survey, and the edge-on disk of AU Mic is clearly detected.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: 5σ sensitivity curves for each target star in the F444W filter (red lines) and F356W filter (blue lines). The sensitivity is given in units of flux contrast in the lower panel. The coronagraph IWA is shown in the gray dashed line, and the separations where only partial coverage exists due square framed observations at multiple roll angles are shown by the gray shaded region. We demonstrate extremely deep limits in absolute flux at close angular separations.
Paper: Probing the Outskirts of M Dwarf Planetary Systems with a Cycle 1 JWST NIRCam Coronagraphy Survey
Authors: Ellis Bogat, Joshua E. Schlieder, Kellen D. Lawson, Yiting Li, Jarron M. Leisenring, Michael R. Meyer, William Balmer, Thomas Barclay, Charles A. Beichman, Geoffrey Bryden, Per Calissendorff, Aarynn L. Carter, Matthew De Furio, Julien H. Girard, Thomas P. Greene, Tyler D. Groff, Jens Kammerer, Jorge Llop-Sayson, Michael W. McElwain, Marcia J. Rieke, Marie Ygouf
Figure caption: 5σ sensitivity curves for each target star in the F444W filter (red lines) and F356W filter (blue lines). The sensitivity is given in units of apparent magnitude in the lower panel. The coronagraph IWA is shown in the gray dashed line, and the separations where only partial coverage exists due square framed observations at multiple roll angles are shown by the gray shaded region. We demonstrate extremely deep limits in absolute flux at close angular separations.
Paper: An Early Look at the Performance of IGRINS-2 at Gemini-North with Application to the Ultrahot Jupiter, WASP-33 b
Authors: Yeon-Ho Choi, Ueejeong Jeong, Jae-Joon Lee, Hyun-Jeong Kim, Heeyoung Oh, Chan Park, Changwoo Kye, Luke Finnerty, Micheal R. Line, Krishna Kanumalla, Jorge A. Sanchez, Peter C. B. Smith, Sanghyuk Kim, Hye-In Lee, Woojin Park, Youngsam Yu, Yunjong Kim, Moo-Young Chun, Jae Sok Oh, Sungho Lee, Jeong-Gyun Jang, Bi-Ho Jang, Hyeon Cheol Seong, Cynthia B. Brooks, Gregory N. Mace, Hanshin Lee, John M. Good, Daniel T. Jaffe, Kang-Min Kim, In-Soo Yuk, Narae Hwang, Byeong-Gon Park, Hwihyun Kim, Brian Chinn, Francisco Ramos, Pablo Prado, Ruben Diaz, John White, Eduardo Tapia, Andres Olivares, Valentina Oyarzun, Emma Kurz, Hawi Stecher, Carlos Quiroz, Ignacio Arriagada, Thomas L. Hayward, Hyewon Suh, Jen Miller, Siyi Xu, Emanuele Paolo Farina, Charlie Figura, Teo Mocnik, Zachary Hartman, Mark Rawlings, Andrew Stephens, Bryan Miller, Kathleen Labrie, Paul Hirst, Byeong-Cheol Lee
Figure caption: Comparison of normalized response functions for IGRINS (red) and IGRINS-2 (blue) obtained from flat lamp frames in the H and K bands with the atmospheric model (gray) used for the analysis. Spectra are obtained from calibration systems after correcting the minor changes in optics. Top panels: the normalized response function of each spectrograph in the H band. IGRINS-2 exhibits improved sensitivity over IGRINS in the entire wavelength range. Bottom panels: the normalized response function of each spectrograph in the K band. These panels show the significant shift in the K band to longer wavelengths in IGRINS-2, covering more CO lines and improving throughput at longer wavelengths.
Paper: An Early Look at the Performance of IGRINS-2 at Gemini-North with Application to the Ultrahot Jupiter, WASP-33 b
Authors: Yeon-Ho Choi, Ueejeong Jeong, Jae-Joon Lee, Hyun-Jeong Kim, Heeyoung Oh, Chan Park, Changwoo Kye, Luke Finnerty, Micheal R. Line, Krishna Kanumalla, Jorge A. Sanchez, Peter C. B. Smith, Sanghyuk Kim, Hye-In Lee, Woojin Park, Youngsam Yu, Yunjong Kim, Moo-Young Chun, Jae Sok Oh, Sungho Lee, Jeong-Gyun Jang, Bi-Ho Jang, Hyeon Cheol Seong, Cynthia B. Brooks, Gregory N. Mace, Hanshin Lee, John M. Good, Daniel T. Jaffe, Kang-Min Kim, In-Soo Yuk, Narae Hwang, Byeong-Gon Park, Hwihyun Kim, Brian Chinn, Francisco Ramos, Pablo Prado, Ruben Diaz, John White, Eduardo Tapia, Andres Olivares, Valentina Oyarzun, Emma Kurz, Hawi Stecher, Carlos Quiroz, Ignacio Arriagada, Thomas L. Hayward, Hyewon Suh, Jen Miller, Siyi Xu, Emanuele Paolo Farina, Charlie Figura, Teo Mocnik, Zachary Hartman, Mark Rawlings, Andrew Stephens, Bryan Miller, Kathleen Labrie, Paul Hirst, Byeong-Cheol Lee
Figure caption: Results of the secondary wavelength calibration. Each point represents the wavelength shift for each spectral order. Since the night-sky frame used for wavelength calibration was taken after our observations, the last frame serves as the reference.
Paper: An Early Look at the Performance of IGRINS-2 at Gemini-North with Application to the Ultrahot Jupiter, WASP-33 b
Authors: Yeon-Ho Choi, Ueejeong Jeong, Jae-Joon Lee, Hyun-Jeong Kim, Heeyoung Oh, Chan Park, Changwoo Kye, Luke Finnerty, Micheal R. Line, Krishna Kanumalla, Jorge A. Sanchez, Peter C. B. Smith, Sanghyuk Kim, Hye-In Lee, Woojin Park, Youngsam Yu, Yunjong Kim, Moo-Young Chun, Jae Sok Oh, Sungho Lee, Jeong-Gyun Jang, Bi-Ho Jang, Hyeon Cheol Seong, Cynthia B. Brooks, Gregory N. Mace, Hanshin Lee, John M. Good, Daniel T. Jaffe, Kang-Min Kim, In-Soo Yuk, Narae Hwang, Byeong-Gon Park, Hwihyun Kim, Brian Chinn, Francisco Ramos, Pablo Prado, Ruben Diaz, John White, Eduardo Tapia, Andres Olivares, Valentina Oyarzun, Emma Kurz, Hawi Stecher, Carlos Quiroz, Ignacio Arriagada, Thomas L. Hayward, Hyewon Suh, Jen Miller, Siyi Xu, Emanuele Paolo Farina, Charlie Figura, Teo Mocnik, Zachary Hartman, Mark Rawlings, Andrew Stephens, Bryan Miller, Kathleen Labrie, Paul Hirst, Byeong-Cheol Lee
Figure caption: Top panel: the median SNR of each band. SNRs are derived from an exposure time of 80 s while observing an A5 star (K = 7.46 mag). Middle panel: seeing variations obtained from DIMM. Bottom panel: air-mass variations during WASP-33 b observations.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Observed, synthetic, and residual spectra for the six EBs. In each subplot, the top panel displays the observed (black points) and synthetic (red line) spectra in the vicinity of the Li I λ6708 line, while the bottom panel shows the same comparison around the Hα lines. The top panel highlights the absorption lines of Li I λ6708 and Ca I λ6718 for both the primary and secondary components, which are marked with the labels “P” and “S,” respectively. In the bottom panel, the Hα emissions for both components are highlighted by the green and magenta hatch-marked areas in the residual spectrum (blue line). To enhance visibility, these observed and residual spectra are offset in the vertical direction. These spectra were acquired at phases near the quadratures, where the spectral lines of the two components display the largest wavelength separation. Lithium absorption is only visible in the spectra of TIC 72696540, from both components, while the Hα filling is only related to the secondary one.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Phased light and RV curves of (a) TIC 17303250, (b) TIC 196817076, (c) TIC 219488423, (d) TIC 252991035, (e) TIC 344753509, and (f) TIC 72696540. For each system, the upper panel displays the observed light curve (black dots) alongside the best-fit model (red line), and the corresponding residuals in the bottom. In the lower panels, primary RVs (blue dots) and secondary RVs (green dots) are shown, along with the RV curve solutions (red lines) and their corresponding residuals at the bottom.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Left panel: the phased secondary eclipse light curves of TIC 72696540 (black and green points), along with the synthetic light curves (red line). Right panel: residuals between green points and the synthetic model.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Mass–radius relationship for TIC 72696540 (left panel) and the other five low-mass stars (right panel).
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Time-series photometry and phased light curves of TIC 17303250.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: (V⊙, U⊙) (left panel) and (V⊙, W⊙) (right panel) diagrams for the six EBs (blue dots). Black asterisks show average velocities of young stellar kinematic groups in the region of the young disk (YD) population (O. J. Eggen 1996). Purple asterisks indicate old kinematic groups.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Fit to the lithium depletion pattern of WLi of the TIC 72696540 components, obtained with the EAGLES code (R. D. Jeffries et al. 2023).
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Position of the primary (blue dot) and secondary (red dot) component of TIC 72696540 in the HR diagram. PMS isochrones and evolutionary tracks from L. Siess et al. (2000) are overlaid as red dashed and purple solid lines; the labels give their age and mass, respectively.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: The fractional deviation of the radii of the primary and the secondary components of the five low-mass binary systems vs. metallicity for 6 and 12 Gyr isochrones, as indicated in the top labels. The shape and colors of the symbols are the same as in Figure 7.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Light curves and posterior distribution of TIC 72696540.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Posterior distribution of TIC 17303250.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Light curves and posterior distribution of TIC 219488423.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Light curves and posterior distribution of TIC 196817076.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Light curves and posterior distribution of TIC 252991035.
Paper: Analysis of Six Long-period Low-mass Eclipsing Binaries
Authors: Yang Pan, Antonio Frasca, Jiaxin Wang, Jianning Fu, Xiaobin Zhang
Figure caption: Light curves and posterior distribution of TIC 344753509.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Differences of DR19 ASPCAP spectroscopic Teff and IRFM temperatures as a function of ASPCAP Teff color coded by metallicity. The left panels show the giants, and the right panels show the dwarfs. Photometric J − Ks and V − Ks temperatures from J. I. González Hernández & P. Bonifacio (2009) can be seen in the top and middle panels, respectively. The bottom panel shows the differences compared to IRFM temperatures calculated from BP − RP colors (L. Casagrande et al. 2021). The solid black line shows the running median value.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Radial velocity (top panels) published in DR19 compared with Gaia DR3 (Gaia Collaboration et al. 2023a), GALAH DR4 (S. Buder et al. 2025), and GES DR5 (S. Randich et al. 2022). The scatter of radial velocities as a function of Teff is shown in the bottom panels.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Position of stars that have parameters and abundances below 8000 K published by Milky Way Mapper in DR19 color coded by [M/H]. Only stars with signal-to-noise ratio (S/N) > 50 per pixel and no BAD flags that are farther than 1000 pc are shown here to reveal the metallicity gradient of our Galaxy.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Raw abundances of giants in the solar neighborhood solar-metallicity sample as a function of Teff. Stars with S/N > 50, no BAD flags, and −0.05 < [M/H] < 0.05 are plotted only. The zero-point offset for giants stars were determined from the 4000–6000 K range. Abundances of Cglobal and Nglobal are from the global fit.
Paper: SDSS-V Milky Way Mapper (MWM): ASPCAP Stellar Parameters and Abundances in SDSS-V Data Release 19
Authors: Szabolcs Mészáros, Paula Jofré, Jennifer A. Johnson, Jonathan C. Bird, Jo Bovy, Andrew R. Casey, Julio Chanamé, Katia Cunha, Nathan De Lee, Peter Frinchaboy, Guillaume Guiglion, Viola Hegedűs, Alex P. Ji, Juna A. Kollmeier, Melissa K. Ness, Jonah Otto, Marc H. Pinsonneault, Alexandre Roman-Lopes, Andrew Saydjari, Amaya Sinha, Ying-Yi Song, Guy S. Stringfellow, Keivan G. Stassun, Jamie Tayar, Andrew Tkachenko, Marica Valentini, Zachary Way, Jörg Weingrill
Figure caption: Main atmospheric parameters comparison with those of derived by D. Souto et al. (2022) as a function of ASPCAP raw Teff values. Top panel: difference of temperatures from D. Souto et al. (2022) and ASPCAP raw Teff values; middle panel: difference of surface gravities from D. Souto et al. (2022) and ASPCAP raw log g values; bottom panel: difference of metallicities from D. Souto et al. (2022) and ASPCAP raw [M/H] values.