adsabs/AstroCLIMB huggingface dataset:
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption: Correlation between the SEXTRACTOR FWHM between Suprime-Cam and HSC for the UDGs in the area of Yagi et al. (2016) that were rejected by the FWHM criterion in our analysis. Our selection limits are the blacked dotted lines, while the red dashed line has unit slope. The FWHM are generally measured as smaller in the Suprime-Cam images.
Paper: Ultradiffuse Galaxies (UDGs) with Hyper Suprime-Cam. I. Revised Catalog of Coma Cluster UDGs 
Authors: Jose Miguel G. Bautista, Jin Koda, Masafumi Yagi, Yutaka Komiyama, Hitomi Yamanoi
Figure caption:  r-band HSC image of SMDG 1306050 + 273627. It is cataloged in Zaritsky et al. (2019), while rejected in this work.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison of the SFRs derived in this work with those from the (a) GSWLC-2 and (b) MPA–JHU catalogs. The typical uncertainties are plotted in the lower-right corner. The residuals (this work − other catalogs) are shown in the upper paneels. The medians and standard deviations of the residuals are given in the upper left corners in the bottom panels. The color code indicates the number density of objects.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: The impact on the estimates of the dust mass (M  d ) from fitting the SED with a different number of upper limits in (solid lines) or by completely dropping the data (dashed lines), for (a) GALEX, (b) WISE, and (c) Herschel. The x-axis shows output − input; the black dotted line shows zero deviation. The legend gives the median and standard deviation of each distribution. The effect on dust mass is moderate for GALEX and WISE but substantial for Herschel. Combining WISE detections in the W3 and W4 bands, together with upper limits in Herschel/SPIRE, can provide useful dust masses after correcting for systematic bias.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison between our measurements and the SDSS modelmag photometry in the (a) u, (b) g, (c) r, (d) i, and (e) z bands. The upper limits (S/N < 2) from our measurements are plotted as red triangles. The upper panels show the differences between the two sets of measurements (this work − modelmag). The dashed line denotes the 1:1 relation. The median and standard deviation derived through survival analysis are shown in the upper left of the bottom panels.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison of the stellar masses derived in this work with those from (a) the GSWLC-2 catalog, (b) the MPA–JHU catalog, and (c) the MPA–JHU catalog, for which our comparison stellar masses were calculated assuming the same star formation history (delayed exponential) as that used in the MPA–JHU catalog. The typical uncertainties are given in the lower-right corner. The residuals (this work − other catalogs) are shown in the upper panels. The medians and standard deviations of the residuals are given in the upper left corners in the bottom panels. The color code indicates the number density of objects.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison of the SFR−M * diagram derived from this work with that from (a) the GSWLC-2 catalog and (b) the MPA–JHU catalog. The distribution of sources from this work is presented as shadowed background contours, overlaid by a colorful contour showing the distribution from the comparison catalogs. The black solid and dashed curves denote the star-forming main sequence and its 1σ scatter (Equation (5)). The gray dotted line marks ﹩\mathrm{log}(\mathrm{sSFR}/{\mathrm{yr}}^{-1})=-12﹩. The top and right panels show the histograms of stellar masses and SFRs, respectively.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison between our measurements and the “total flux” measurements of the 2MASS XSC in the (a) J, (b) H, and (c) K  s  bands. The upper limits (S/N < 2) from our measurements are shown in red triangles. The upper panels show the differences between the two sets of measurements (this work − 2MASS). The dotted lines give the quadrature sum of the typical uncertainties of the two sets of measurements. The median and standard deviation derived through survival analysis are shown in the upper left of the bottom panels.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison between our measurements and the 2MASS PSF-fitting magnitudes in the (a) J, (b) H, and (c) K  s  bands. The upper limits (S/N < 2) from our measurements are shown in red triangles. The upper panels show the differences between the two sets of measurements (this work − 2MASS). The dotted lines give the quadrature sum of the typical uncertainties of the two sets of measurements. The median and standard deviation derived through survival analysis are shown in the upper left of the bottom panels.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison between our measurements and those from the GALEX catalog in the (a) FUV and (b) NUV bands. The upper limits (S/N < 2) from our measurements are shown in red triangles. The upper panels show the differences between the two sets of measurements (this work − GALEX). The dotted lines give the quadrature sum of the typical uncertainties of the two sets of measurements. The median and standard deviation derived through survival analysis are shown in the upper left of the bottom panels.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Comparison of the main sequence derived in this work with those from Saintonge et al. (2016) and Renzini & Peng (2015). Our main sequence is derived following the method in Saintonge et al. (2016).
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: Panel (a) shows the predicted connectivity of Solar Orbiter traced back to the solar surface on an ADAPT magnetic field map at a Sun time (plasma release time) of 2022 March 3 at 12:00:00 UT, 6 hr after the start of the first remote-sensing window, with a predicted solar wind release time of 2022 March 5 at 07:27:28 UT. The positions of the green and red connectivity points are calculated by assuming fast and slow solar wind speeds of 800 and 300 km s−1, respectively. The red arrows and circle show the evolution in the magnetic connectivity that occurs prior to the start of the remote-sensing window that begins on 2022 March 3 at 06:00 UT. White (black) represents positive (negative) photospheric magnetic field polarities, and the sub-spacecraft point is indicated by the blue cross. The black line encompasses the region of the solar disk that is visible from Solar Orbiter, and the red dotted line shows the location of the HCS determined from the coronal field model. Panel (b) shows the predicted connectivity of Solar Orbiter during RSW2. The labels are the same as for panel (a).
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: Remote-sensing data taken at the beginning of RSW1 of the Slow Wind SOOP. Panel (a) shows an EUI/FSI 174 Å image taken at the start of the first 1 hr high-resolution observation window. The FOVs of EUI/HRI, PHI/HRT, and SPICE are given by the blue, red, and green boxes, respectively. The green dashed box shows the FOV of the SPICE data in panel (e) cropped to remove the bright dumbbell at the top of the raster. Panel (b) shows the FOVs on the corresponding 193 Å image taken by the Atmospheric Imaging Assembly (Lemen et al. 2012) on board SDO (Pesnell et al. 2012) with photospheric magnetic polarities overlaid from the Helioseismic and Magnetic Imager (Scherrer et al. 2012), where red (blue) represents positive (negative) field with a saturation of ± 300 G. Panels (c)–(e) show the EUI/HRI 174 Å, the PHI/HRT line-of-sight magnetic field, and the SPICE Mg VIII/Ne VIII spectral window at wavelength position 23. In panel (d), white (black) represents positive (negative) field with a saturation level of ± 50 G, and ARs 12957, 12959, and 12961 are labeled in white.
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: The target selection for the high-resolution remote-sensing instruments on board Solar Orbiter on 2022 March 3 and 5. The left panels show the low-latency EUI/FSI 304 Å images using JHelioviewer (Müller et al. 2017) from 2022 February 27 at 08:50 UT and 2022 March 1 at 03:50 UT projected to 2022 March 3 at 06:00 UT and 2022 March 4 at 06:00 UT, respectively. The white boxes show the approximate size and location of the FOVs of EUI/HRI and PHI/HRT (large), as well as those of SPICE (small). The red (green) circles represent the distribution of connectivity points predicted for slow (fast) wind from the connectivity tool, and the white line shows the position of the HCS. The grid labels are shown in Carrington coordinates. The text in the bottom right gives the feature triplet provided to Solar Orbiter, which includes Carrington latitude and longitude, as well as the epoch of the coordinates. The magnetic differential rotation model was applied to track the feature. The right panels show the resulting EUI/FSI and HRI 174 Å observations on 2022 March 3 and 5. The distributions of the postobservation connectivity points are also shown.
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: High-resolution data taken during RSW2 of the Slow Wind SOOP on 2022 March 18 (panels (a)–(c)) and 2022 March 19 (panels (f)–(h)). The FOVs of EUI/HRI, PHI/HRT, and SPICE are shown in blue, green, and red on EUI/FSI 174 Å and SDO/AIA 193 Å data, similarly to Figure 5.
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: Hinode/EIS observations taken during RSW2 of the Slow Wind SOOP. The panels from left to right show the SDO/AIA 193 Å images, with the red dashed box showing the target and FOV for Hinode/EIS, Fe XII intensity, Doppler velocity, and nonthermal velocity maps. In panel (h), the nonthermal velocity maps only show pixels with negative Doppler velocity.
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: The target selection for the high-resolution observations taken during RSW2 on 2022 March 17 and 18. The left panels show the low-latency EUI/FSI 174 Å images from 2022 March 13 at 10:30 UT and March 15 at 08:30 UT, respectively. The right panels show the EUI/FSI and HRI 174 Å observations taken on 2022 March 17 and 19. The labels are the same as described in Figure 3.
Paper: Slow Solar Wind Connection Science during Solar Orbiter’s First Close Perihelion Passage
Authors: Stephanie L. Yardley, Christopher J. Owen, David M. Long, Deborah Baker, David H. Brooks, Vanessa Polito, Lucie M. Green, Sarah Matthews, Mathew Owens, Mike Lockwood, David Stansby, Alexander W. James, Gherardo Valori, Alessandra Giunta, Miho Janvier, Nawin Ngampoopun, Teodora Mihailescu, Andy S. H. To, Lidia van Driel-Gesztelyi, Pascal Démoulin, Raffaella D'Amicis, Ryan J. French, Gabriel H. H. Suen, Alexis P. Rouillard, Rui F. Pinto, Victor Réville, Christopher J. Watson, Andrew P. Walsh, Anik De Groof, David R. Williams, Ioannis Zouganelis, Daniel Müller, David Berghmans, Frédéric Auchère, Louise Harra, Udo Schuehle, Krysztof Barczynski, Éric Buchlin, Regina Aznar Cuadrado, Emil Kraaikamp, Sudip Mandal, Susanna Parenti, Hardi Peter, Luciano Rodriguez, Conrad Schwanitz, Phil Smith, Luca Teriaca, Cis Verbeeck, Andrei N. Zhukov, Bart De Pontieu, Tim Horbury, Sami K. Solanki, Jose Carlos del Toro Iniesta, Joachim Woch, Achim Gandorfer, Johann Hirzberger, David Orozco Súarez, Thierry Appourchaux, Daniele Calchetti, Jonas Sinjan, Fatima Kahil, Kinga Albert, Reiner Volkmer, Mats Carlsson, Andrzej Fludra, Don Hassler, Martin Caldwell, Terje Fredvik, Tim Grundy, Steve Guest, Margit Haberreiter, Sarah Leeks, Gabriel Pelouze, Joseph Plowman, Werner Schmutz, Sunil Sidher, William T. Thompson, Philippe Louarn, Andrei Federov
Figure caption: Overview of IRIS observations during the RSW1 and RSW2 on 2022 March 3 and 18. The panels show (from left to right): a full-disk context AIA 193 Å image with the FOV of the IRIS SJI and spectrograph raster overlaid, an SJI in the 1400 Å filter with the spectrograph raster FOV overlaid, and images of Si IV intensity, Doppler shift velocity, and nonthermal velocity.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: Example of preprocessing a W2 image before aperture photometry. (a) Source detection and deblending the target (red cross) from other sources; a nearby contaminating source is masked (orange ellipse). (b) The final mask combines the detection mask (all sources except the target segment) and the deblend mask (if a contaminant is deblended). (c) The final image used for aperture photometry, generated using the surface brightness profile model of the target to interpolate the masked pixels with the model and adding noise.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: The impact on the estimates of (a) M * and (b) SFR from fitting the SED by (top) using upper limits and (bottom) completely dropping them in 2MASS+WISE+Herschel/SPIRE (red), GALEX (blue), and Herschel/SPIRE (green). The x-axis shows output − input; the black dotted line denotes zero deviation. The legend gives the median and standard deviation of each distribution.
Paper: Panchromatic Photometry of Low-redshift, Massive Galaxies Selected from SDSS Stripe 82
Authors: Yang A. Li, Luis C. Ho, Jinyi Shangguan, Ming-Yang Zhuang, Ruancun Li
Figure caption: The distribution of stellar mass (Salim et al. 2018) and redshift for galaxies in Stripe 82. We color code the targets by (a) the number density of SDSS galaxies in each stellar mass–redshift bin and (b) the detection rate in Herschel/SPIRE 250 μm (HELP catalog; Shirley et al. 2021). Galaxies with S/N > 2 are considered detections. We bin stellar mass in steps of 0.5 dex and redshift in steps of 0.01. The detection fraction is defined as the ratio between the number of detections over the number of galaxies in each bin. The cuts of redshift and stellar mass for our sample are shown as black dash lines (see the text for more details).