adsabs/AstroCLIMB huggingface dataset:
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Example of coadded error spectra in log (y-axis), obtained by stacking 50,000 individual error spectra. Here, f(λ) denotes the flux of error spectra after the moving average. The regions of skylines, marked by red brackets, are discarded. The range devoid of skylines is utilized for PCA.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Comparison between NN-predicted distance modulus, (m − M)predict, and reference distance modulus, (m − M)true. The reference distance modulus is from GCs, Sgr, and dwarf galaxy member stars that can have a more precise distance measurement from their hosts or stream tracks. Left: all validation stars. Right: stars with distance modulus error < 0.5, which correspond to a precision of 25% in distance.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: External validations for the distance measurements of X.-X. Xue et al. (2014; top left), C. Wang et al. (2022; top middle), M. Zhang et al. (2024; top right and bottom left), F. Anders et al. (2022; bottom middle) and X. Zhang et al. (2023; bottom right). For the top left and middle panels, most stars are matched to the member star list of Sgr. The top right panel is based on matched member stars to a few GCs and dwarf galaxies. The bottom left panel is based on DESI Year-1 BHB stars. For the bottom, middle, and right panels, we only present the validation based on GCs and Sgr member stars. For the top middle, bottom middle, and right panels, only stars flagged as good measurements are plotted. In all panels, the red solid line marks y = x to guide the eye.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Comparison between our distance measurements in this paper (x-axis) and the spectrophotometric distance measurements in six previous studies, including SEGUE K giants (X.-X. Xue et al. 2014, top left), LAMOST OB stars (M. Xiang et al. 2021, top middle), LAMOST VAC (C. Wang et al. 2022, top right), the more recent measurement for DESI EDR based on the Payne (M. Zhang et al. 2024, bottom left), photoastrometric distances of Gaia EDR3 (F. Anders et al. 2022, bottom middle), and distances measured from Gaia BP/RP spectra (X. Zhang et al. 2023, bottom right). For the top right, bottom middle, and bottom right panels, we only compare those stars that are flagged as good measurements. In all panels, the red solid line marks y = x to guide the eye.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: HR diagram based on the full test sample. The x-axis of two panels is the color index derived from the mean magnitudes of the Gaia photometry in the BP and RP bands. The y-axis of the left panel represents the NN-predicted absolute magnitude, MG,NN. The y-axis of the right panel shows the absolute magnitude deduced from Gaia parallax, MG,geo, without any cuts on parallax error. Negative parallaxes are excluded from the right plot.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Distribution of single stars (black dots) and binaries (red dots) in the HR diagram. Binaries are identified by our Gaussian mixture model (Equation (9)) with Pbinary > 0.7. Stars plotted in the figure are based on a subset of the test sample with precise parallax measurements of ω/σω > 10. The x-axis is the color index based on Gaia photometry in BP and RP bands. The y-axis is the geometric absolute magnitude MG,geo based on Gaia parallax. The distribution of binaries shows a clear shift from single stars by ∼0.75 mag.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Top: distribution of relative distance uncertainty of the total sample. Middle: relative distance uncertainty as a function of the S/N. The red line shows the median value of the relative error at various S/N. Bottom: relative distance uncertainty of the total sample as a function of distance; the distance uncertainty is derived by the method of Section 3.3. The red line shows the median value of the relative error at various distances.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Median distance measurement errors obtained by Monte Carlo sampling the error spectra (see Section 3.3), reported as a function of the S/N of the stellar spectra. Black and red curves are for stars with ﹩{\mathrm{log}}\,g\lt 3.8﹩ and ﹩{\mathrm{log}}\,g\gt 3.8﹩, respectively.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Comparison between (m − M)predict and (m − M)true based on all DESI Year-1 BHB stars. The reference distance modulus, (m − M)true, is from DESI Year-1 BHB VAC.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Black line: distribution of heliocentric distance of the full sample. Red line: distribution of heliocentric distances of stars with relative distance error smaller than 25%.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Distributions of (m − M)predict predicted by NN (the green histogram) and (m − M)geo derived from Gaia parallax (the black filled histogram). Each panel shows an individual GC, a dwarf galaxy, or a given distance bin of the Sgr. The red vertical dashed line marks the reference distance modulus of the parent object, and the blue vertical dashed line marks the median of the distance modulus predicted by NN. When the number of member stars is too few, we do not show the blue vertical line. The text in each panel indicates the name of the object and its distance.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Comparison between MG,NN and MG,geo. Here, MG,NN is obtained in Section 4.1, and we only plot a subset of the test sample with precise parallax measurement ω/σω > 10, based on which we can deduce precise MG,geo. We apply the method of Section 5 to distinguish binaries and single stars. The left plot is for single stars, and the right plot is for binary stars. In both panels, the red solid line shows the y = x diagonal line, and the red dashed line has an offset of 0.75 mag above the diagonal line.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Equal-mass binary fraction reported as a function of [Fe/H] and [α/Fe]. This is based on a subset of stars having precise Gaia parallax measurements, i.e., ω/σω > 10. Error bars represent the 1σ scatter among 50 bootstrap subsamples.
Paper: SpecDis: Value Added Distance Catalog for 4 Million Stars from DESI Year-1 Data
Authors: Songting Li, Wenting Wang, Sergey E. Koposov, Ting S. Li, Youjia Wu, Monica Valluri, Joan Najita, Carlos Allende Prieto, Amanda Byström, Christopher J. Manser, Jiaxin Han, Carles G. Palau, Hao Yang, Andrew P. Cooper, Namitha Kizhuprakkat, Alexander H. Riley, Leandro Beraldo e Silva, Jessica Nicole Aguilar, Steven Ahlen, David Bianchi, David Brooks, Todd Claybaugh, Axel de la Macorra, John Della Costa, Arjun Dey, Peter Doel, Jaime E. Forero-Romero, Enrique Gaztañaga, Satya Gontcho A Gontcho, Gaston Gutierrez, Klaus Honscheid, Mustapha Ishak, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Anthony Kremin, Martin Landriau, Laurent Le Guillou, Michael Levi, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Nathalie Palanque-Delabrouille, Will Percival, Claire Poppett, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Eusebio Sanchez, David Schlegel, Michael Schubnell, Hee-Jong Seo, Joseph Harry Silber, David Sprayberry, Gregory Tarlé, Benjamin Alan Weaver, Rongpu Zhou, Hu Zou
Figure caption: Relationships between [Fe/H], Teff, and the coefficients of three principal components. C1, C2, and C100 represent the coefficients of the first, second, and 100th PCs. Here [Fe/H] and Teff are from RVS table.
Paper: The RR Lyrae Luminosity Metallicity Relation Revisited
Authors: Ata Sarajedini
Figure caption: Comparisons of the fits (dashed lines) to the fitted parameters (dots) for the case of Equation (2) in terms of MF606W(TO), where F606W is the corresponding filter in the system of the Advanced Camera for Surveys onboard the Hubble Space Telescope using the DSEP isochrones.
Paper: The RR Lyrae Luminosity Metallicity Relation Revisited
Authors: Ata Sarajedini
Figure caption: Weighted least-square fits of the MV(RR) zero points as a function of the slope of each relation using the DSEP and BaSTI models for all of the clusters in Table 1 and in the cases without (w/o) 47 Tuc.
Paper: The RR Lyrae Luminosity Metallicity Relation Revisited
Authors: Ata Sarajedini
Figure caption: Variation of ΔV(TO – HB) with [Fe/H] as modeled in Equation (3) for the MV(RR) ∼ [Fe/H] slopes and zero points listed in the second and fifth columns, respectively, of Table 3 using the DSEP isochrones at [α/Fe] = +0.40 dex (without 47 Tuc). The open circles are the observed ΔV(TO – HB) values from A. Rosenberg et al. (1999) at the average [Fe/H] for each cluster in Table 1. The ages are given in Gyr.
Paper: The RR Lyrae Luminosity Metallicity Relation Revisited
Authors: Ata Sarajedini
Figure caption: Comparisons of the fits (dashed lines) to the fitted parameters (dots) for the case of Equation (2) using the DSEP isochrones.
Paper: The RR Lyrae Luminosity Metallicity Relation Revisited
Authors: Ata Sarajedini
Figure caption: Comparisons of the fits (dashed lines) to the fitted parameters (dots) for the case of Equation (2) using the BaSTI isochrones.
Paper: KMT-2018-BLG-0029Lb and OGLE-2019-BLG-0960Lb: Mass Measurements for Two Super-Earth Microlensing Planets
Authors: Keming Zhang, 可名 张, Sean K. Terry, Joshua S. Bloom, B. Scott Gaudi, Jessica R. Lu
Figure caption: Caustic representations for the inner and outer solutions for KMT-2018-BLG-0029. The vertical dashed lines mark the locations of the planetary caustic/cusp located at s − 1/s, which are equidistant to the source trajectory marked with the downwards arrow. Top: exact caustic representation. Bottom: caustic representations under the Chang–Refsdal Lens approximation, where the inner and outer solutions are shown to be exactly symmetrical.