adsabs/AstroCLIMB huggingface dataset:
Paper: Spectropolarimetric Inversion in Four Dimensions with Deep Learning (SPIn4D). I. Overview, Magnetohydrodynamic Modeling, and Stokes Profile Synthesis
Authors: Kai E. Yang, 凯 杨, Lucas A. Tarr, Matthias Rempel, S. Curt Dodds, Sarah A. Jaeggli, Peter Sadowski, Thomas A. Schad, Ian Cunnyngham, Jiayi Liu, 嘉奕 刘, Yannik Glaser, Xudong Sun, 旭东 孙
Figure caption: Panels (a) and (b) display the continuum opacity tables derived from the MURaM and SIR models, respectively. Panel (c) illustrates the ratio of these opacity tables, highlighting the pressure and temperature ranges with colored lines for Case 1 at t = 5.4 hr across various ﹩{\mathrm{log}}_{10}\tau ﹩ layers.
Paper: The Catalogue of Gamma-Ray Burst Observations by HEPD-01 in the 0.3–50 MeV Energy Range
Authors: S. Bartocci, R. Battiston, S. Beolè, W. J. Burger, D. Campana, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubüser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, L. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: (a) Example of the fitting procedure. Dots and error bars correspond to the measured rate and the related uncertainty. The blue, dashed line is the initial first-degree polynomial that best fits the whole set of 60 data points within the window. Data points colored in red, which significantly deviate from the initial model, are identified as outliers according to the procedure described in the main text. The blue, solid line corresponds to the second first-degree polynomial fit, carried out by excluding outlier points. As the sum of normalized residuals S is equal to 42.5, the window is flagged as anomalous. (b) Rate signal upon subtraction of the background polynomial model. Data points colored in red are identified as outliers according to the procedure described in the main text. The red, dashed vertical line corresponds to the trigger time of GRB 220624A (S. Lesage & C. Meegan 2022).
Paper: The Catalogue of Gamma-Ray Burst Observations by HEPD-01 in the 0.3–50 MeV Energy Range
Authors: S. Bartocci, R. Battiston, S. Beolè, W. J. Burger, D. Campana, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubüser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, L. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: Time-resolved and detection profiles for the 12 GRBs after background subtraction and scaling: GRB 181222B, GRB 190114C, GRB 190129B, GRB 190305A, GRB 190928A, GRB 200412B, GRB 200422A, GRB 200826B, GRB 201009A, GRB 210702A, GRB 211211A, and GRB 220624A. The plots show the recorded rate by HEPD-01 superimposed to the light curves provided by dedicated GRB detectors, whose energy ranges are provided in the plot legends. Each panel corresponds to a specific GRB event (see labels on top of the plots) with time profiles shown relative to the trigger time T 0 and corrected for the light travel time between the two compared instruments. The light curves for FERMI GBM or Swift-BAT (in green) and SPI-ACS (in red) are normalized to the maximum of the HEPD-01 data to ensure comparability across different detector sensitivities. Each curve is detrended via a suitable background model tailored for that specific time region, which leads to an enhancement of the accuracy of the observed GRB signal. Shaded gray areas represent the time interval considered for the extraction of the GRB temporal features.
Paper: The Catalogue of Gamma-Ray Burst Observations by HEPD-01 in the 0.3–50 MeV Energy Range
Authors: S. Bartocci, R. Battiston, S. Beolè, W. J. Burger, D. Campana, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubüser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, L. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: Diagram of the method used to collect data from similar orbits, in order to determine typical background fluctuations and shapes. Overlapping windows, each having a duration of 60 s, are depicted in the middle, each shifted by 15 s. A specific test window at time t 0 is highlighted in blue. A time span of approximately 5 days and corresponding to the satellite’s recurrence time is highlighted. The time intervals of ±30 minutes around the times t 0 ± 5 × K × 86,400, with K ranging from 1 to 3 (three on the right and three on the left), and which are considered to assess background data, are highlighted in green. Data outside these regions (light-red area) are neglected. The final selection, which relies on geographical distance, yields a single orbit segment within each green time frame.
Paper: The Catalogue of Gamma-Ray Burst Observations by HEPD-01 in the 0.3–50 MeV Energy Range
Authors: S. Bartocci, R. Battiston, S. Beolè, W. J. Burger, D. Campana, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubüser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, L. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: Correlation analyses between HEPD-01 and dedicated GRB detectors for the 12 GRBs after background subtraction and scaling: GRB 181222B, GRB 190114C, GRB 190129B, GRB 190305A, GRB 190928A, GRB 200412B, GRB 200422A, GRB 200826B, GRB 201009A, GRB 210702A, GRB 211211A, and GRB 220624A. Each plot correlates the GRB detector count scaled after background subtraction as in Figure 4 vs. the rate measured by HEPD-01 (in Hz). Instrument and energy ranges are reported on the axis. The color scale represents the post-trigger time T 0, considering the light travel time between the two compared instruments. All plots show positive correlation coefficients.
Paper: The Catalogue of Gamma-Ray Burst Observations by HEPD-01 in the 0.3–50 MeV Energy Range
Authors: S. Bartocci, R. Battiston, S. Beolè, W. J. Burger, D. Campana, P. Cipollone, A. Contin, M. Cristoforetti, C. De Donato, C. De Santis, A. Di Luca, F. M. Follega, G. Gebbia, R. Iuppa, A. Lega, M. Lolli, M. Martucci, G. Masciantonio, M. Mergè, M. Mese, C. Neubüser, R. Nicolaidis, F. Nozzoli, A. Oliva, G. Osteria, F. Palma, B. Panico, F. Perfetto, A. Perinelli, P. Picozza, E. Ricci, L. Ricci, M. Ricci, S. B. Ricciarini, Z. Sahnoun, U. Savino, V. Scotti, M. Sorbara, A. Sotgiu, R. Sparvoli, P. Ubertini, V. Vilona, S. Zoffoli, P. Zuccon
Figure caption: The figure shows a comparison of the effective area of the detector at different incident angles using the HEPD-01 Monte Carlo simulation. The effective area (in cm2) is plotted as a function of energy (in MeV) for five different angles of incidence: 0° (black), 30° (red), 50° (blue), 70° (green), and 90° (magenta). Each data point represents the measured effective area at a specific energy.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Gallery of observations of the HT Lup system. (a) ALMA 1.25 mm continuum observations of HT Lup AB from N. T. Kurtovic et al. (2018). Contour curves correspond to the 5σ, 28σ and 150σ levels, showcasing the extension of the dust disk of HT Lup A as well as the location of HT Lup B. (b) Hα (6563 Å) image of HT Lup B after HRSDI processing. (c) Hβ (4861 Å) image of HT Lup B after HRSDI processing. (d) [O I] (6300 Å) image of HT Lup B after HRSDI processing. All the MUSE images were equally normalized for visualization purposes.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Hα profiles for the three data sets of HT Lup B. Labels correspond to the time, in minutes, after the first observation of each data set. Dashed horizontal lines mark the 0 km s−1 velocity, corresponding to the Hα wavelength in vacuum (6563 Å).
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Hα profiles for the three available data sets of HT Lup A. Labels correspond to the time in minutes after the first observation of each data set. Dashed horizontal lines mark the 0 km s−1 point, corresponding to the Hα wavelength in vacuum (6563 Å). Besides the higher Hα flux level on HT Lup A, the lines exhibit a clear distinction from those from the secondary. In particular, the emission lines at the first epoch showcase a slightly redshifted absorption feature, not found on any other observations. The data was carefully inspected to discard any artificial origin for this feature, such as saturation of the data. The variation of the line flux follows an opposite trend to that of HT Lup B; while the lower flux in the second epoch appears to indicate a more relaxed, quiescent state for HT Lup B, for HT Lup A emission increases compared to the first, possibly indicating different accretion events taking place in HT Lup A and B.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: [O I]λ6300 line profile fits for the three available data sets of HT Lup B. Black lines correspond to the mean line profile from each data set. For the first epoch, the best fit consists of a double Gaussian profile, while both data sets of the second epoch are better fitted by a single component. Green and blue dashed lines represent the HVC and LVC, respectively, as defined in Section 5.4. Dashed horizontal lines mark the 0 km s−1 point.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Hα flux variability as a function of time. Each measurement corresponds to the difference in flux for an individual pair of lines from the full set of observations, divided by the minimum flux of the pair. The color of each point represents the σ-distance between the lines used to compute the flux variation. Gray points indicate a value of σ < 3, considered to show no flux variation given the uncertainties on the flux measurement for each pair. Colored points correspond to values of σ ≥ 3, indicating real flux variation.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Example of the flux variation for an injected fake source with a Gaussian Hα line profile. (A) Result for one cube of the first epoch. (B) Same as (A) but for a cube of the second epoch. For each case the line was modeled so as to have a similar flux to the one of HT Lup B at the respective epoch, to better estimate the impact on a comparable source. For both cases, the post-processed profiles remain almost identical to the preprocessed ones, with an almost constant oversubtraction along the full wavelength range being clearly identifiable on the line wings.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: [O I]λ6300 profiles for the three available data sets of HT Lup B. Labels correspond to the time in minutes after the first observation of each data set. Only lines with an SNR higher than 10 at the peak of the emission were included for the analysis. Dashed horizontal lines mark the 0 km s−1 point, corresponding to the [O I] wavelength in vacuum (6300 Å).
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Left: possible orbits for HT Lup B around HT Lup A, generated with the orbitize! Python package considering the five astrometry points presented in Table 1. Right: separation (ρ) and PAs for the retrieved orbits at different epochs, compatible with the available astrometry for HT Lup B.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Same as Figure 10 but after being corrected for the constant flux loss observed initially.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Corner plot for the HT Lup B orbital parameters from the orbitize! Python package, considering the five astrometry points presented in Table 1.
Paper: VLT/MUSE Detection of Accretion/Ejection Associated with the Close Stellar Companion in the HT Lup System
Authors: Sebastián Jorquera, Mickaël Bonnefoy, Laura M. Pérez, Gaël Chauvin, Adrian Aguinaga, Catherine Dougados, Rémi Julo, Dorian Demars, Sean M. Andrews, Luca Ricci, Zhaohuan Zhu, Nicolas T. Kurtovic, Nicolás Cuello, Xue-Ning Bai, Til Birnstiel, Cornellis Dullemond, Viviana V. Guzmán
Figure caption: Average Hβ line profiles in HT Lup B for each data set. Each profile was computed considering only observations with SNR > 5 for the Hβ line.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: Upper panel: the semimajor effective radius vs. stellar mass relation at 1 < z < 1.3 for PSBs (green, this sample) and star-forming (blue) and quiescent (red) 3D-HST galaxies. Symbol shapes indicate isolated (circles) and interacting (stars) PSBs. The best-fitting relations for each population are shown as dashed lines and typical error bars are indicated in the lower right corner. Lower panel: deviations from the quiescent size–mass relation. The error on the best-fitting quiescent relation is shown as a shaded region in dark red and the scatter of quiescent galaxies around the best-fitting quiescent relation is in light red. On average, the PSBs in this sample are more compact than both star-forming and quiescent galaxies.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: Upper panels: median surface mass density profiles along the semimajor axes for (﹩\mathrm{log}({M}_{* }/{M}_{\odot })\lt 11.2﹩) PSBs (black) vs. mass-matched quiescent (left) and star-forming (right) galaxies. The PSB population scatter is shown as a shaded region in light green and the scatter among the quiescent and star-forming galaxies is indicated by dashed lines. The HWHM of the HST/F110W PSF is shown as a gray band. The impact of PSF is negligible beyond a > 1 kpc . Lower panels: residuals of subtracting the median quiescent (left) and star-forming (right) median profiles from the median PSB profile. The intrinsic scatter of the differences between PSB and quiescent/star-forming galaxies is shown as a shaded region in light green in each panel.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: Upper left: original image. Upper middle: best-fitting 2D Sérsic model. Upper right: residual image of an example PSB with clear tidal features. The color map is chosen so that positive pixel values are black, negative pixel values are red, and zero pixel values are white. The red solid ellipse in each upper panel traces the largest annulus used for profile extraction. The red dashed circle in each upper panel traces the aperture size of the DESI fiber centered on the pointing of this target. The yellow polygons with hatches in each upper panel mark the regions in the image data that are masked out during the model fitting. Lower left: radial surface brightness profiles as a function of the semimajor axis of the best-fitting ellipse of original data (top; black), best-fitting model (top; pink), and residual (bottom; black) extracted with annular apertures centered on the PSB. Lower right: radial surface brightness profiles of the best-fitting Sérsic model (pink) and the same model with the residual added (black), using the method in D. Szomoru et al. (2012). There is minimal difference between the Sérsic half-light radius (black solid line) and the residual-corrected value.
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: An example of spectrophotometric fitting for one of the PSBs. In the upper left panel, we show the best-fitting models (green) and the observed photometry (g/r/z/W1/W2, black). In the upper right panel, we show the median (black solid line) and 68% confidence interval (gray region) SFH. The time since quenching is defined as the lookback time where the sSFR drops below the threshold of ﹩\mathrm{log}(\mathrm{sSFR}[{\mathrm{yr}}^{-1}])\lt -10﹩. We overplot the median (green dashed line) and 68% confidence interval (light green region) of the quenching time. In the lower panel, we show the smoothed observed spectrum (5 pixel boxcar smoothed, black) and the best-fitting model spectrum (green).
Paper: DESI Massive Poststarburst Galaxies at z ∼ 1.2 Have Compact Structures and Dense Cores
Authors: Yunchong Zhang, David J. Setton, Sedona H. Price, Rachel Bezanson, Gourav Khullar, Jeffrey A. Newman, Jessica Nicole Aguilar, Steven Ahlen, Brett H. Andrews, David Brooks, Todd Claybaugh, Axel de la Macorra, Biprateep Dey, Peter Doel, Enrique Gaztañaga, Satya Gontcho A Gontcho, Jenny E. Greene, Stephanie Juneau, Robert Kehoe, Theodore Kisner, Mariska Kriek, Joel Leja, Marc Manera, Aaron Meisner, Ramon Miquel, John Moustakas, Francisco Prada, Graziano Rossi, Eusebio Sanchez, Michael Schubnell, Małgorzata Siudek, Justin Spilker, David Sprayberry, Katherine A. Suess, Gregory Tarlé, Hu Zou
Figure caption: The surface mass density in the central 1 kpc vs. stellar mass relation for PSBs (green) and star-forming (blue) and quiescent (red) 3D-HST galaxies (upper panel), and the residuals from the quiescent relation (lower panel). The plotting convention is the same as in Figure 3. Despite their more compact sizes, the PSBs in this sample have similar central surface mass densities as the quiescent galaxies.