adsabs/AstroCLIMB huggingface dataset:
Paper: Spectro-temporal Evolution of 4U 1702-429 Using AstroSat-NICER
Authors: Suchismito Chattopadhyay, Ranjeev Misra, Soma Mandal, Akash Garg, Sanjay K. Pandey
Figure caption: The best-fitted PDS for Obs. 1, Obs. 2, and NICER. Blue points represent the NICER PDS, and red points represent the LAXPC PDS.
Paper: Spectro-temporal Evolution of 4U 1702-429 Using AstroSat-NICER
Authors: Suchismito Chattopadhyay, Ranjeev Misra, Soma Mandal, Akash Garg, Sanjay K. Pandey
Figure caption: The left panels show the simultaneous, background-subtracted LAXPC 20 (top) and SXT light curve (bottom) for Obs. 1 of 4U 1702-429 in the energy ranges of 3–20 keV and 0.3–8 keV, respectively. The right panels show the simultaneous LAXPC 20 (top), SXT (middle), and NICER (bottom) light curve for Obs. 2 using energy bands of 3–20 keV, 0.3–8 keV, and 0.2–12 keV, from top to bottom panel, respectively. All the light curves have the same binning time of 2.378 s.
Paper: Spectro-temporal Evolution of 4U 1702-429 Using AstroSat-NICER
Authors: Suchismito Chattopadhyay, Ranjeev Misra, Soma Mandal, Akash Garg, Sanjay K. Pandey
Figure caption: The top panel shows the hardness intensity diagram for the Obs. 1 and 2 using background-subtracted light curves of 3–8 keV (soft band) and 8–20 keV (hard band) with time bin 256 s using LAXPC 20 only, whereas the bottom panel shows the position of Obs 1 and 2 in comparison to the MAXI hardness intensity diagram with a time bin of 2 days. The intensity is defined to be the sum of the count rates in the given two energy bands, and the hardness ratio is defined to be the ratio of the counts in the hard band with respect to the soft band.
Paper: Spectro-temporal Evolution of 4U 1702-429 Using AstroSat-NICER
Authors: Suchismito Chattopadhyay, Ranjeev Misra, Soma Mandal, Akash Garg, Sanjay K. Pandey
Figure caption: The upper panel shows the ratios of the spectral fitting using cons∗tbabs∗(thcomp∗bbodyrad). High excess residuals can be seen at 2 keV, between 5 and 10 keV, and beyond 12 keV. The bottom panel shows the ratios of the spectral fitting using cons∗tbabs∗(thcomp∗diskbb). The excess residuals are still visible.
Paper: Spectro-temporal Evolution of 4U 1702-429 Using AstroSat-NICER
Authors: Suchismito Chattopadhyay, Ranjeev Misra, Soma Mandal, Akash Garg, Sanjay K. Pandey
Figure caption: The observed rms (top) and lag (bottom) for the kHz QPO ∼800 Hz. The model lag and rms variation uses the variation in the heating rate of the corona. The light blue points indicate the rescaled rms variation. The solid line represents the model prediction for a corona of size 30 km and η = 0.1.
Paper: Spectro-temporal Evolution of 4U 1702-429 Using AstroSat-NICER
Authors: Suchismito Chattopadhyay, Ranjeev Misra, Soma Mandal, Akash Garg, Sanjay K. Pandey
Figure caption: The left and right panels show the spectra for Obs. 1 and Obs. 2, respectively. Both spectra have been fitted using the model cons∗tbabs∗(Gaussian+diskbb+ireflect∗thcomp∗bbodyrad), and the bottom panels show Δχ.
Paper: Protoplanetary Disks around Sun-like Stars Appear to Live Longer When the Metallicity is Low 
Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkić, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes
Figure caption: Left: CMD of the stars in NGC 346 (G. De Marchi et al. 2011a). All magnitudes are corrected for extinction. Objects with excess emission in Hα at the 4σ level or higher are shown as open circles. A total of 694 of them (red dots) also have Hα excess emission with EW in excess of 20 Å or more than 50 Å for stars hotter than 10,000 K. Squares correspond to objects with Hα excess emission and EW of less than 50 Å that are potential Be stars. The thick black dashed line corresponds to the 50% completeness limit of the photometry in the V and I bands (E. Sabbi et al. 2007). The majority of other stars in the field (gray dots) do not show Hα excess emission. Thin green dashed lines correspond to isochrones from J. Tang et al. (2014) for Z = 0.002 and ages of 0.125, 0.25, 0.5, 1, 2, 4, 8, 16, and 32 Myr from right to left. The arrows show representative reddening vectors for color excess E(V − I) = 0.5 and two values of the total-to-selective extinction ratio: R = 3.1 (standard Galactic extinction law, top arrow), and R = 4.5 as measured in the low-metallicity massive starburst cluster 30 Dor (bottom arrow). Right panel: H-R diagram of the stars with Hα excess at the 4σ level or higher. Thick solid lines show the evolutionary tracks from the Pisa group (S. Degl'Innocenti et al. 2008; E. Tognelli et al. 2011) for metallicity Z = 0.002 and masses from 0.5 to 4 M ⊙, as indicated. The corresponding isochrones are shown as thin dashed lines, for the same ages as in the left panel. Note that the constant logarithmic age step has been selected such that the typical distance between isochrones is larger than the uncertainties (indicated by the typical error bars in the bottom-left corner of the H-R diagram). The purple polygon is discussed in Section 5.4.
Paper: Protoplanetary Disks around Sun-like Stars Appear to Live Longer When the Metallicity is Low 
Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkić, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes
Figure caption: Spectra of sources 9884 (top panel) and 20408 (bottom panel). For each star, we display the 1D spectrum (after background subtraction) and associated 1σ uncertainties (which are derived from standard error propagation through the reduction pipeline). In the bottom panel, we show the 2D-rectified trace. The panels on the right-hand side show the HST F658N (Hα) and the NIRCam F444W filter negative images, with the three nodding positions of the NIRSpec slitlet array aperture shown in blue. There are three nodding positions, namely “abc,” “bcd,” and “cde,” with the footprints of the five individual microshutters labeled a to e in the figure. Note that isolated bright pixels, such as those appearing in the 2D-rectified trace in the top panel near 1.8 μm and 2.6 μm, are the result of flags in the pipeline processing to exclude spurious pixels (e.g., hot pixels, cosmic-ray hits, saturation, no linearity correction, etc.). Once flagged, the pixels are excluded from the analysis and do not have any effect on the extracted one-dimensional spectra (same panel in Figure 1) that are used in this work.
Paper: Protoplanetary Disks around Sun-like Stars Appear to Live Longer When the Metallicity is Low 
Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkić, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes
Figure caption: Calibrated, background-subtracted spectra of seven PMS and three MS representative stars. Object numbers correspond to Table 1. To improve visibility, the spectra are shifted vertically by offsets of (11.5, 10, 8.5, 7, 5.5, 4, 3, 2.2, 1.6, 1.1) × 10−18 erg cm−2 s−1 Å−1. The vertical scale in this figure is compressed and the H absorption lines in the spectra of MS stars, although present, might be difficult to see. For a clearer view, see Figure 3.
Paper: Protoplanetary Disks around Sun-like Stars Appear to Live Longer When the Metallicity is Low 
Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkić, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes
Figure caption: PMS evolutionary tracks from E. Tognelli et al. (2011) for a 1 M ⊙ star and two different metallicities, as indicated. Numbers along the tracks correspond to PMS ages in Myr. At Z = 1/8 Z ⊙, the transition from the bottom of the Hayashi track to the MS occurs earlier and more rapidly than at Z ⊙. For reference, we also show the error bars from the right panel of Figure 6.
Paper: Protoplanetary Disks around Sun-like Stars Appear to Live Longer When the Metallicity is Low 
Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkić, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes
Figure caption: SEDs (fitted continua) of the dereddened sources registered at 1.75 μm. The spectra of PMS stars are shown individually (thick color lines as per the legend), while the three MS stars are averaged together (gray dashed line), as in Figure 3. The thin lines correspond to theoretical model spectra for metallicity [M/H] = −0.5 and T eff = 4500 K, 6500 K, and 8000 K, respectively.
Paper: Spectro-temporal Evolution of 4U 1702-429 Using AstroSat-NICER
Authors: Suchismito Chattopadhyay, Ranjeev Misra, Soma Mandal, Akash Garg, Sanjay K. Pandey
Figure caption: The fractional rms and time-lag variation with LAXPC 20 within 3–20 keV and NICER within 1–7 keV at 9.37 Hz for Obs. 2. Solid points in the top panel show the rescaled rms variation, and the light points show the original variation that has been obtained from the observation. The solid line represents the model prediction for a corona of size 30 km and η = 0.3.
Paper: Protoplanetary Disks around Sun-like Stars Appear to Live Longer When the Metallicity is Low 
Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkić, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes
Figure caption: Comparison of PMS and MS spectra. The spectrum of PMS star 12559 (black line) is compared with the mean of the three MS spectra in our sample (red line), and with a model atmosphere with physical parameters appropriate for the MS objects (blue line).
Paper: Protoplanetary Disks around Sun-like Stars Appear to Live Longer When the Metallicity is Low 
Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkić, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes
Figure caption: Localized H2 excitation lines around source 40571. Left: source spectra along the seven individual pixel rows of the rectified trace, without background subtraction. Right: projected position of the source in the microshutter. The v = 1 → 0  S (1) excitation line is stronger at the specific location of the source, while nebular lines are present across the full slit length.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Distributions of observed properties (upper panels) and spectral properties (lower panels) of ELGs as a function of Coeff1 (x-axis) and Coeff2 (y-axis). In the upper panels, the left panel shows the number of sources in each Coeff1 and Coeff2 bin. The second to the fourth panels show the median values of the redshifts, WISE 1 mag, and g-band magnitude, respectively. The lower panels from left to right show the median values of the p-value, with the null hypothesis being that the F  d  model does not provide a better fit than the F  s  model, velocity dispersion σ  s , velocity offset (Δv), and [O II] luminosity respectively. We note that for clarity, pixels with a number of sources lower than 10, which occupy ∼0.7% of the total number of sources, are not displayed.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Distribution of ELGs in the PCA Coeff1 (x-axis) and Coeff2 (y-axis) space. ELGs are separated into four regions, narrow (N), broad (B), double-peak (D), and outlier (O), by the two dashed lines (Coeff2 = 0.15 × Coeff1 − 0.25 and Coeff1 = 0) and with background colors being blue, green, orange, and pink respectively. The value shown in each region indicates the fraction of total sources in the region, and the top and right panels show the number distributions of the four types as a function of Coeff1 and Coeff2, respectively. The median values of the uncertainties of Coeff1 and Coeff2 are 0.17 and 0.16, respectively, as shown in the lower-left corner. The uncertainties of the PCA coefficients of each spectrum are estimated by perturbing the spectrum with the observed spectral noise 1000 times and obtaining the corresponding coefficients and the standard deviations.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Example spectra of DESI ELGs as a function of Coeff1 and Coeff2. The values shown on the top left corner in each panel are (Coeff1, Coeff2) values of the ELG. The gray spectrum is the observed spectrum, the black curve is the PCA reconstructed spectrum based on the first two eigenspectra, and the uncertainty array is in brown. The background colors of the panels indicate the locations of the ELGs in the Coeff1 and Coeff2 space, as shown in Figure 2.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Mean spectrum and PCA eigenspectra of DESI ELGs. The top panel shows the mean spectrum, and the second to fifth panels show the eigenspectra ordered by their explained variance listed in each panel. The two vertical dashed lines indicate the wavelengths of the [O II] doublet.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Stellar mass and SFR of ELGs as a function of Coeff1 (x-axis) and Coeff2 (y-axis). The colors in the left and right panels indicate the median stellar mass and SFR of ELGs, respectively. For clarity, pixels with the number of sources lower than five, which occupy ∼0.6% of the total number of sources, are not displayed.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Correlation between ΔA, ﹩{\rm{\Delta }}{\mathrm{log}}_{10}\,\mathrm{SFR}﹩, and line profiles. The upper panels show the median ΔA (left) and ﹩{\rm{\Delta }}{{\rm{log}}}_{10}\,{\rm{SFR}}/{M}_{\odot }\,{{\rm{yr}}}^{-1}﹩ (right) as a function of Coeff1 and Coeff2. The lower panels show the fractions of ELGs with ΔA > 0.1 (left) and ﹩{\mathrm{\Delta log}}_{10}\,\mathrm{SFR}\gt 0.35﹩ (right) within nine Coeff1–Coeff2 regions from narrow (blue), broad (green), to double-peak (orange), respectively. The color boxes show the same measurements for a control sample consisting of star-forming galaxies selected to have similar stellar mass, redshifts, and sizes as the DESI ELGs. The uncertainties are based on bootstrapping the sample 1000 times.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Correlations between stellar mass, SFR, and Coeff1. The upper panels show the number distributions of ELGs with different Coeff1 values indicated by blue (−1 < Coeff1 < −0.5), cyan (−0.5 < Coeff1 < 0), green (0 < Coeff1 < 0.5), and orange (0.5 < Coeff1 < 1). The vertical color dashed lines reflect the median stellar mass of the ELGs within the corresponding Coeff1 bin. The three panels from left to right show the results for ELGs at three redshift bins from z = 0.6 to z = 1.63. The lower panels show the SFR as a function of stellar mass with colors indicating Coeff1. The small data points are individual ELGs and the large data points with uncertainty are the median SFR as a function of stellar mass for each Coeff1 bin. The uncertainties are estimated based on bootstrapping the sample 1000 times. The gray dashed lines in the lower panels are the median relationship based on galaxies in the COSMOS-SFG sample within the same redshift regions.
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Example images (3″ × 3″) of DESI ELGs with different ΔA values. Each column shows the HST ACS F814W images of four randomly selected DESI ELGs within the ΔA selection, as shown at the top of the column. The ΔA values increase from left to right, respectively. The values listed on the lower-left corner of the images are the ﹩{\mathrm{\Delta log}}_{10}\,\mathrm{SFR}﹩ of the ELGs and the values on the right are (Coeff1, Coeff2). The color dots on the lower-right corner indicate the spectral regions of the ELGs, with blue, green, and orange for narrow, broad, and double-peak regions, respectively. The gray circle indicates the size of the DESI fiber (1.″5 in diameter).
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Median ΔA values and ﹩{\mathrm{\Delta log}}_{10}\,\mathrm{SFR}﹩ of star-forming galaxies as a function of g − r, r − z, and g-band fiber magnitude (gfib). Galaxies are selected with ﹩{\mathrm{log}}_{10}{M}_{* }/{M}_{\odot }\gt 9﹩, 1.1 < z photo < 1.63, and g > 20 from the COSMOS2020 catalog with HST ACS morphology measurements. The upper panels are median ΔA values as a function of galaxy colors with gfib < 23.6 (left), 23.6 < gfib < 24.1 (middle), and 24.1 < gfib < 24.6 (right). The lower panels are median ﹩{\mathrm{\Delta log}}_{10}\,\mathrm{SFR}﹩ as a function of galaxy colors with gfib < 23.6 (left), 23.6 < gfib < 24.1 (middle), and 24.1 < gfib < 24.6 (right).
Paper: DESI Emission-line Galaxies: Unveiling the Diversity of [O II] Profiles and Its Links to Star Formation and Morphology
Authors: Ting-Wen Lan, J. Xavier Prochaska, John Moustakas, Małgorzata Siudek, J. Aguilar, S. Ahlen, D. Bianchi, D. Brooks, T. Claybaugh, S. Cole, K. Dawson, A. de la Macorra, P. Doel, J. E. Forero-Romero, E. Gaztañaga, S. Gontcho A Gontcho, G. Gutierrez, J. Guy, K. Honscheid, R. Kehoe, T. Kisner, A. Lambert, M. Landriau, A. Meisner, R. Miquel, A. Muñoz-Gutiérrez, J. A. Newman, C. Poppett, F. Prada, G. Rossi, E. Sanchez, M. Schubnell, H. Seo, D. Sprayberry, G. Tarlé, B. A. Weaver, H. Zou
Figure caption: Relation between ΔA and galaxy elongation of ELGs with ﹩10\lt {\mathrm{log}}_{10}\,{M}_{* }/{M}_{\odot }\lt 10.5﹩. Top: normalized number distributions of ELGs in the B1 and B2 regions (green) and in the D1 and D2 regions (orange) as a function of galaxy elongation. Middle: ΔA distribution as a function of galaxy elongation for the two ELG samples. Bottom: fractions of ELGs with ΔA > 0.1 as a function of galaxy elongation for the two ELG samples. The uncertainties are estimated by bootstrapping the sample 1000 times.