adsabs/AstroCLIMB huggingface dataset:
Paper: Systematic Multiepoch Monitoring of LkCa 15: Dynamic Dust Structures on Solar System Scales
Authors: Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Comparison of observed multiepoch ﹩{L}^{{\prime} }﹩ reconstructions to expectations for best-fit three-point-source and polar Gaussian ring models (both static and dynamic). The top row shows images reconstructed from the highest signal-to-noise ﹩{L}^{{\prime} }﹩ observations (orange; a subset of those shown in Figure 2). The following rows show images reconstructed from the best-fit dynamic polar Gaussian ring (Dynamic PGR), dynamic three-point-source (Dynamic 3PS), static polar Gaussian ring (Static PGR), and static three-point-source (Static 3PS), with Gaussian noise added to match the scatter in the observations.
Paper: Systematic Multiepoch Monitoring of LkCa 15: Dynamic Dust Structures on Solar System Scales
Authors: Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: SQUEEZE-reconstructed images from individual epochs listed in Table 1. Each reconstruction includes an unresolved central model component with fractional flux f * that represents the star, with a location marked by the +. The panel color indicates the observing wavelength.
Paper: Systematic Multiepoch Monitoring of LkCa 15: Dynamic Dust Structures on Solar System Scales
Authors: Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Best-fit polar Gaussian ring models fit to all data obtained at the H band (left), K  s  band (center), and ﹩{L}^{{\prime} }﹩ band (right). In each panel, the location of the central star is marked with a +, and the star accounts for fractional flux f *. The top three rows of Table 3 list the best-fit parameters for each data set.
Paper: Systematic Multiepoch Monitoring of LkCa 15: Dynamic Dust Structures on Solar System Scales
Authors: Steph Sallum, Josh Eisner, Andy Skemer, Ruth Murray-Clay
Figure caption: Best-fit polar Gaussian ring models for each individual ﹩{L}^{{\prime} }﹩ epoch. In each panel, the location of the central star is marked with a +, and the star accounts for fractional flux f *. Table 3 lists the best-fit parameters for each data set.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: The fractions of the stellar population with mass-weighted (top) and light-weighted (bottom) ages divided by three mass bins. These fractions are measured in the same way as in Figure 2. The errors are measured by the confidence interval of the fraction for a beta distribution, which depends on the sample size.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: This figure shows the light-curve evolution of SN 2018cni in BgVri bands. In the right Y-axis, absolute magnitudes in the corresponding BgVri bands are presented.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: (a) Location of SN 2018cni in its host galaxy. This image was acquired in V-band with the 1 m LCO telescope on 2018 July 17. (b) SN 2020kyg and its host galaxy NGC 5012. This image was taken in V-band with the 1 m LCO telescope on 2020 June 27.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Light-curve evolution of SN 2020kyg in BgVri bands. Absolute magnitudes in BgVri bands for SN 2020kyg are shown on the right Y-axis.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Comparison of the normalized light curves of SNe 2018cni and 2020kyg with a few other well-studied Type Iax SNe.
Paper: The Origin of Star Formation in Early-type Galaxies Inferred from Spatially Resolved Spectroscopy
Authors: Yun Hee Lee, Ho Seong Hwang, Narae Hwang, Jong Chul Lee, Ki-Beom Kim
Figure caption: Radial profiles of stellar metallicity for four types of galaxies in different mass bins. These profiles are measured in the same way as in Figure 4 but are displayed by the three mass bins. The metallicity is estimated by mass-weighted (top) and light-weighted (bottom) ways, respectively. The errors are calculated by the bootstrap method.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: This figure presents the pseudobolometric light curves of SNe 2018cni and 2020kyg. The pseudobolometric light curves of SNe 2002cx, 2005hk, 2008ha, and 2010ae are included for comparison. The figure shows that SN 2018cni belongs to the bright Type Iax SNe, whereas SN 2020kyg conforms to the fainter class of Type Iax SNe.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Color curves of SNe 2018cni and 2020kyg and their comparison with the color evolution of other Type Iax SNe.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Top panel: the best-fit function for SN 2018cni (red) compared to the N1-def and N3-def pure deflagration density structure at ﹩{t}_{\exp }\,=\,{t}_{0}\,=\,100\,{\rm{s}}﹩. The gray lines indicate the boundaries of the fitting layers for the corresponding chemical abundance models. Bottom panel: the best-fit chemical abundance structure from the TARDIS fitting process for the spectral sequence of SN 2018cni. The profile of the radioactive 56Ni shows the mass fractions at ﹩{t}_{\exp }\,=\,100\,{\rm{s}}﹩.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: (a) This figure represents the comparison between spectra of SNe 2018cni, 2002cx, and 2005hk. (b) This figure shows the comparison between the spectra of SNe 2020kyg, 2008ha, 2010ae, and 2019gsc. The comparison features in both figures are marked with shaded bars.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: This figure depicts the evolution of blackbody temperature and radius obtained through SuperBol. The evolution of the blackbody temperature is the same for both SNe, whereas the blackbody radius is higher for SN 2018cni than SN 2020kyg.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Comparison of the bolometric light curves of different proposed models with the pseudobolometric light curves of SNe 2018cni and 2020kyg.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Spectral sequence of SN 2020kyg at −4.0, −3.1, 5.9, 15.8, and 34.9 days since maximum.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Spectral evolution of SN 2018cni from −2 to 55 days since maximum.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Fitting of the spectra of SN 2020kyg using TARDIS is shown in this figure. Here, gray lines display the spectra of the SN and red lines present the respective models.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: This figure presents the spectral fitting of SN 2018cni using TARDIS. The gray and blue lines show the SN spectra and the corresponding models, respectively.
Paper: Observational Properties of a Bright Type lax SN 2018cni and a Faint Type Iax SN 2020kyg
Authors: Mridweeka Singh, Devendra. K. Sahu, Raya Dastidar, Barnabás Barna, Kuntal Misra, Anjasha Gangopadhyay, D. Andrew Howell, Saurabh W. Jha, Hyobin Im, Kirsty Taggart, Jennifer Andrews, Daichi Hiramatsu, Rishabh Singh Teja, Craig Pellegrino, Ryan J. Foley, Arti Joshi, G. C. Anupama, K. Azalee Bostroem, Jamison Burke, Yssavo Camacho-Neves, Anirban Dutta, Lindsey A. Kwok, Curtis McCully, Yen-Chen Pan, Matt Siebert, Shubham Srivastav, Tamás Szalai, Jonathan J. Swift, Grace Yang, Henry Zhou, Nico DiLullo, Jackson Scheer
Figure caption: Pseudobolometric light curves of SNe 2018cni and 2020kyg obtained through SuperBol along with their respective Arnett–Valenti model (dashed line) fits.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: The left panel is a 2D histogram of the stars in the CMD with PMs selected and background-subtracted. The red dashed line represents the CMD filter moved upward by 0.5 mag. The right panel is a 2D histogram of the PMs after CMD selection and background subtraction. The red dashed line represents the PM filters in this space. Both of the diagrams are smoothed with a 2D Gaussian kernel of σ = 1 pixel. The blue polygons represent the CMD and PM selections applied to the stream and off-stream regions.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: Same analysis as for the leading tail but for the trailing tail. Top: weighted map and lateral profile. Middle: stream overdensities in CMD and PM space. Bottom: adopted member candidate stars compared to the CMD and PM filters.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: Illustration of why we set G 0 < 19.3 mag in Figure 4. Based on the model, we select nearby stars on the sky (blue dots in the top panel) and further in PM space (cyan dots in the bottom left panel). These stars are compared to M3 on a CMD (bottom right panel), and it can be found that G 0 < 19.3 mag is able to discard most of the contaminants.
Paper: Mass Distribution for Single-lined Hot Subdwarf Stars in LAMOST
Authors: Zhenxin Lei, Ruijie He, Péter Németh, Xuan Zou, Huaping Xiao, Yong Yang, Jingkun Zhao
Figure caption: Example of comparison synthetic SED with observed photometric fluxes. Flux density is multiplied by wavelength to the power of 3 to eliminate the steep slope of SED. The black solid curve denotes the synthetic SED calculated based on the atmospheric parameters obtained from LAMOST spectra fitting, while magenta crosses denote the observed photometric fluxes with different filters retrieved from VOSA.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: Heliocentric distance variation along the stream. Green dots represent the model stream. Blue triangles show our estimates of the distance of each stream segment in a certain R.A. range. The blue circle indicates M3.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: The left panel is a CMD of M3 (blue dots) and Svöl (red stars). The stream stars are all placed at M3's distance. The right panel shows the model stream (green dots) and Svöl (red stars) in planes of decl., heliocentric distance, ﹩{\mu }_{\alpha }^{* }﹩, and μ  δ  as a function of R.A. from top to bottom.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: Blue points show the candidate stars of the leading tail with weights >0.91. The red dashed line in the left panel represents the CMD filter moved upward by 0.5 mag (same as Figure 7). The red dashed lines in the right panels represent the PM filters.
Paper: The Spectacular Tidal Tails of Globular Cluster M3 (NGC 5272)
Authors: Yong Yang, Jing-Kun Zhao, Xin-Zhe Tang, Xian-Hao Ye, Gang Zhao
Figure caption: The green dots show the model stream’s radial velocity as a function of R.A. The member stars in Table 1 are plotted as the black points. The blue circle indicates M3.
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: Ionized gas spectra of (a) UVISTA 169610, (b) UVISTA 174150, and (c) UVISTA 77854 around the Hα, [N II]λ6550,λ6585 emission, in observed wavelength. The raw spectrum is shown in gray lines, and the black solid line in each panel shows the ionized gas spectrum smoothed with 29 pixels. For UVISTA 169610 and 77854, we fit six Gaussians to the ionized gas spectrum, accounting for both broad- (solid) and narrow- (dashed) line components of Hα (green), [N II]λ6550 (blue), and [N II]λ6585 (orange). The thick purple line is the sum of the six Gaussians, smoothed in the same way as the observed spectrum. For UVISTA 169610, the fitted standard deviations of the broad- and narrow-line components are σ br = 707 km s−1 (FWHMbr = 2.35σ br = 1661 km s−1) and σ nr = 176 km s−1, respectively. For UVISTA 77854, the fitted standard deviations are σ br = 400 km s−1 and σ nr = 131 km s−1. (d) The UVJ locations of the three galaxies and their SFH from Prospector fitting on a logarithmic time axis. We find that the ionized outflows found in UVISTA 169610 and 77854 are most likely driven by AGNs, given their high [N II]/Hα ratios and the kinematics of the broad emission components (FWHM > 1000 km s−1). UVISTA 174150, which is the reddest and quenched earlier, does not show any emission features, which might be because the AGN has already blown away all the ionized gas.
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: Left: formation timescale ﹩{t}_{50}^{90}﹩ of massive quiescent TNG100 galaxies (﹩10.6\lt \mathrm{log}({M}_{\mathrm{stellar}}/{M}_{\odot })\lt 12.0﹩) at z ∼ 1.5 as a function of their quenching epoch (z quench). Galaxies are color-coded by their ﹩{t}_{50}^{90}﹩ normalized by the age of the Universe at their quenching epoch. For comparison, the blue hatched bar indicates the 16th–84th percentile range of the ﹩{t}_{50}^{90}﹩ of 12 rapidly quenched UVISTA galaxies. We select 12 quiescent TNG100 galaxies that have the shortest ﹩{t}_{50}^{90}﹩, marked with pentagons. Right: SFH of 12 TNG100 galaxies at z ∼ 1.5 that are most rapidly formed. The green solid line shows the SFH derived from the age distribution of all stellar particles within 3 R eff, and the hatched gray histogram shows the SFH of stellar particles formed ex situ and later accreted. The formation timescales are shown as orange horizontal bars. The quenching epoch z quench and the mass fraction of the stellar particles formed ex situ f ex situ are given in the right corner of each panel. We mark the epoch when the kinetic AGN feedback is turned on for each galaxy with the magenta arrows. It seems clear that kinetic AGN feedback is the key driver of the rapid quenching in TNG100. While major mergers appear to have triggered the starbursts in five of 12 rapidly quenched analogs in TNG100, the starbursts in the rest are likely triggered by other mechanisms not involving major mergers.
Paper: Rapid Quenching of Galaxies at Cosmic Noon
Authors: Minjung Park, Sirio Belli, Charlie Conroy, Sandro Tacchella, Joel Leja, Sam E. Cutler, Benjamin D. Johnson, Erica J. Nelson, Razieh Emami
Figure caption: Left: 3D-DASH cutout images of seven of our 12 rapidly quenched candidates that are covered in the 3D-DASH survey. The box size is 3″. The redshift of the galaxy (z), its effective radius (R e), and the Sérsic index (n Sersic) are shown in lower right corner of each panel. UVISTA 199028 appears to be extremely compact, resulting in a bad fit using GALFIT. Right: size–mass relation for six of our UVISTA rapidly quenched candidates. UVISTA 199028 is plotted as a dashed arrow. The gray horizontal line indicates the PSF FWHM = 0.″18, below which the size of the galaxy might not be well resolved (the measured size being an upper limit). The red dashed line and the hatch region indicate the size–mass relation for quiescent galaxies at z = 1.75 from van der Wel et al. (2014), while the relation for quiescent galaxies at z = 1.25 is shown as the red solid line and the shade. The stellar masses of the galaxies in this plot are derived using FAST, provided in Muzzin et al. (2013a), and the sizes are corrected to “rest-frame” sizes, to be consistent with van der Wel et al. (2014). We find that most of our UVISTA rapidly quenched candidates with size measurements seem to be more compact than normal quiescent galaxies at their respective redshifts.