adsabs/AstroCLIMB huggingface dataset:
Paper: Radial and Local Density Dependence of Star Formation Properties in Galaxy Clusters from the Hyper Suprime-Cam Survey
Authors: Hung-Yu Jian, Lihwai Lin, Bau-Ching Hsieh, Keiichi Umetsu, Carlos Lopez-Coba, Masamune Oguri, Connor Bottrell, Yoshiki Toba, Yusei Koyama, Yu-Yen Chang, Tadayuki Kodama, Yutaka Komiyama, Surhud More, Kai-Yang Lin, Atsushi J. Nishizawa, Ichi Tanaka
Figure caption: Median log sSFR of star-forming galaxies as a function of the normalized host-centric radius r  p /r 200m  (top), and the sSFR reduction (Δ) of star-forming galaxies compared to galaxies in the mean field (bottom) in three redshift ranges. Four mass ranges are denoted by yellow, green, blue, and purple solid lines. The vertical black dashed lines mark the cluster border. Due to different mass completeness limits at different redshifts, only four, three, and two mass ranges are displayed in low, medium, and high redshifts, respectively. The shaded regions indicate the error bars estimated using bootstrap resampling from 200 runs. It is evident that there is a reduction of ∼0.1 dex inside clusters, and the reduction appears to be weakly dependent on the host-centric radius. The results suggest a slow quenching mechanism operating in the overdense regions.
Paper: Radial and Local Density Dependence of Star Formation Properties in Galaxy Clusters from the Hyper Suprime-Cam Survey
Authors: Hung-Yu Jian, Lihwai Lin, Bau-Ching Hsieh, Keiichi Umetsu, Carlos Lopez-Coba, Masamune Oguri, Connor Bottrell, Yoshiki Toba, Yusei Koyama, Yu-Yen Chang, Tadayuki Kodama, Yutaka Komiyama, Surhud More, Kai-Yang Lin, Atsushi J. Nishizawa, Ichi Tanaka
Figure caption: The normalized color-coded density plot for defining green valley galaxies using all galaxies on the SFR–M * plane in three redshift ranges. Each panel’s blue and red open circles represent the median SFR of star-forming and quiescent galaxies. In addition, the blue and red solid lines denote the best-fit results of the median SFR of the star-forming and quiescent galaxies, respectively. The region enclosed by two parallel green lines is the transition area occupied by the green valley galaxies. The green valley zone is defined as 2.0σ away from the star-forming main sequence with a width of 0.4 dex, where σ is the standard deviation of the SFR for star-forming galaxies. The mass completeness limits for star-forming and quiescent galaxies in the corresponding redshift range are marked by the vertical light-blue and red dashed lines, respectively.
Paper: Ultra-deep Keck/MOSFIRE Spectroscopic Observations of z ∼ 2 Galaxies: Direct Oxygen Abundances and Nebular Excitation Properties
Authors: Leonardo Clarke, Alice Shapley, Ryan L. Sanders, Michael W. Topping, Tucker Jones, Mariska Kriek, Naveen A. Reddy, Daniel P. Stark, Mengtao Tang
Figure caption: Comparison of the direct oxygen abundance measurements of our stacks with strong-line indicators from Curti et al. (2020) in orange and Bian et al. (2018) in purple. Strong-line indicators are plotted in solid lines over their quoted metallicity ranges, and extrapolations are shown by dashed lines. We also display z > 1 galaxies from the literature with direct oxygen abundance measurements as blue points (see Sanders et al. 2020, 2023a). Finally, we show the median relation of local H II regions (see Sanders et al. 2017) as a solid black curve, with the 1σ spread illustrated as black dotted curves.
Paper: Ultra-deep Keck/MOSFIRE Spectroscopic Observations of z ∼ 2 Galaxies: Direct Oxygen Abundances and Nebular Excitation Properties
Authors: Leonardo Clarke, Alice Shapley, Ryan L. Sanders, Michael W. Topping, Tucker Jones, Mariska Kriek, Naveen A. Reddy, Daniel P. Stark, Mengtao Tang
Figure caption: Two-dimensional and one-dimensional spectra of the eight [O III] auroral targets in this study. These spectral plots span from 4335 Å to 4370 Å, covering the Hγ and [O III]λ4364 emission lines. The solid black line shows the flux density, and the shaded gray spectrum is the error on the flux density. We detect [O III]λ4364 (labeled with an orange dotted line) in COSMOS-18812 and GOODS-N-8240; however, we report emission blueward of 4364 Å in the GOODS-N 6699 and 14595 spectra.
Paper: Radial and Local Density Dependence of Star Formation Properties in Galaxy Clusters from the Hyper Suprime-Cam Survey
Authors: Hung-Yu Jian, Lihwai Lin, Bau-Ching Hsieh, Keiichi Umetsu, Carlos Lopez-Coba, Masamune Oguri, Connor Bottrell, Yoshiki Toba, Yusei Koyama, Yu-Yen Chang, Tadayuki Kodama, Yutaka Komiyama, Surhud More, Kai-Yang Lin, Atsushi J. Nishizawa, Ichi Tanaka
Figure caption: The color-coded density plot on the SFR vs. M * plane for clusters (N ≥ 15) in three redshift ranges. Two parallel green lines denote the green valley region defined in Figure 1. The vertical light-blue and red dashed lines give the mass completeness limits. It is can be seen that the star-forming main sequence of cluster galaxies is closer to the green valley zone than that of all galaxies in Figure 1, implying an SFR depletion of cluster galaxies.
Paper: Ultra-deep Keck/MOSFIRE Spectroscopic Observations of z ∼ 2 Galaxies: Direct Oxygen Abundances and Nebular Excitation Properties
Authors: Leonardo Clarke, Alice Shapley, Ryan L. Sanders, Michael W. Topping, Tucker Jones, Mariska Kriek, Naveen A. Reddy, Daniel P. Stark, Mengtao Tang
Figure caption: N/O vs. oxygen abundance for stacks 1 and 3 as well as for GOODS-N-8240 compared to local Universe H II-region measurements from Pilyugin et al. (2012).
Paper: A Severe Challenge to the Modified Newtonian Dynamics Phenomenology in Our Galaxy
Authors: Man Ho Chan, Ka Chung Law
Figure caption: The colored lines (solid: p-family; dotted: δ-family) represent the MOND RC gradient dV/dR against the disk scale length a  d  for different disk total mass M  d,10, where M  d,10 = M  d /1010 M ⊙. The red, black, and blue dashed lines respectively indicate the best-fit RC gradient, its 5σ upper bound (without considering systematic uncertainties), and its 2σ upper bound (including 1% systematic uncertainties) from the MWRC data. The shaded region is the region ruled out by the 5σ upper bound.
Paper: A Severe Challenge to the Modified Newtonian Dynamics Phenomenology in Our Galaxy
Authors: Man Ho Chan, Ka Chung Law
Figure caption: The black lines (assuming an exponential baryonic disk) and green lines (assuming a small baryonic disk with radius <17 kpc) indicate the functions of dV/dR against p (left) and δ (right). The red solid line indicates the best-fit RC gradient and the shaded regions bounded by the red dotted lines represent the parameter space ruled out at 5σ based on the MWRC data. The blue shaded regions indicate the parameter space ruled out at 1σ based on the Mercury precession data (Chan & Lee 2023).
Paper: A Severe Challenge to the Modified Newtonian Dynamics Phenomenology in Our Galaxy
Authors: Man Ho Chan, Ka Chung Law
Figure caption: The black dots with error bars represent the data of the MWRC for R = 17–23 kpc (Ou et al. 2023). The red solid line indicates the best-fit RC gradient dV/dR = −5.07 km s−1 kpc−1. The red dotted lines indicate the 5σ upper and lower bounds of the best-fit RC gradients.
Paper: The Polarized Cosmic Hand: IXPE Observations of PSR B1509−58/MSH 15−52 
Authors: Roger W. Romani, Josephine Wong, Niccoló Di Lalla, Nicola Omodei, Fei Xie, C.-Y. Ng, Riccardo Ferrazzoli, Alessandro Di Marco, Niccoló Bucciantini, Maura Pilia, Patrick Slane, Martin C. Weisskopf, Simon Johnston, Marta Burgay, Deng Wei, Yi-Jung Yang, Shumeng Zhang, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Nicoló Cibrario, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Ioannis Liodakis, Philip Kaaret, Vladimir Karas, Dawoon E. Kim, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Grzegorz Madejski, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Riccardo Middei, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Chiara Oppedisano, Luigi Pacciani, Alessandro Papitto, George G. Pavlov, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgró, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Silvia Zane
Figure caption: Overview of the MSH 15−52 complex, the “Cosmic Hand.” The background energy-coded CXO image (0.5–1.2 keV = red, 1.2–2 keV = green, 2–7 keV = blue) shows low-energy (red/yellow) emission from thermal gas in G320.4−1.2 and harder nonthermal emission from the PWN. Superposed are IXPE 2–8 keV PCUBE-derived bars showing the polarization degree (PD, bar length in the legend is for PD = 1) and projected magnetic field direction on a 30″ grid. Yellow bars show >5σ polarization detections, thick white bars >3σ, and thin white bars >2σ. In general, the magnetic field appears to follow the thumb, fingers, and other linear structures (see Figure 2 for region labels). Particularly strong polarization is associated with the arc, especially to the northeast of the pulsar and with the far southeast end of the jet. We have used a flux cut to trim anomalous vectors near the field-of-view edge.
Paper: The Polarized Cosmic Hand: IXPE Observations of PSR B1509−58/MSH 15−52 
Authors: Roger W. Romani, Josephine Wong, Niccoló Di Lalla, Nicola Omodei, Fei Xie, C.-Y. Ng, Riccardo Ferrazzoli, Alessandro Di Marco, Niccoló Bucciantini, Maura Pilia, Patrick Slane, Martin C. Weisskopf, Simon Johnston, Marta Burgay, Deng Wei, Yi-Jung Yang, Shumeng Zhang, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Nicoló Cibrario, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Ioannis Liodakis, Philip Kaaret, Vladimir Karas, Dawoon E. Kim, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Grzegorz Madejski, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Riccardo Middei, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Chiara Oppedisano, Luigi Pacciani, Alessandro Papitto, George G. Pavlov, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgró, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Silvia Zane
Figure caption: Inner region of MSH 15−52 from 0.5–8 keV CXO data, centered on the pulsar and smoothed with a 1″ Gaussian kernel. Note the subluminous zone (marked by an ellipse 2/3 of the zone size), the symmetry axis (red arrow), the bright polar outflow to the northwest, and the fainter, more diffuse outflow to the southeast. The magenta square marks the central pixel of the PCUBE polarization map, Figure 1 (approximating IXPE's resolution); “simultaneous fit” pixels are half this size, Figure 4. The “Inner Arc” passes through the northwest polar outflow, while the “Outer Arc” is partly visible to the north.
Paper: The Polarized Cosmic Hand: IXPE Observations of PSR B1509−58/MSH 15−52 
Authors: Roger W. Romani, Josephine Wong, Niccoló Di Lalla, Nicola Omodei, Fei Xie, C.-Y. Ng, Riccardo Ferrazzoli, Alessandro Di Marco, Niccoló Bucciantini, Maura Pilia, Patrick Slane, Martin C. Weisskopf, Simon Johnston, Marta Burgay, Deng Wei, Yi-Jung Yang, Shumeng Zhang, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Nicoló Cibrario, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Ioannis Liodakis, Philip Kaaret, Vladimir Karas, Dawoon E. Kim, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Grzegorz Madejski, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Riccardo Middei, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Chiara Oppedisano, Luigi Pacciani, Alessandro Papitto, George G. Pavlov, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgró, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Silvia Zane
Figure caption: Top: IXPE phase bin PA estimates (green; q and u values available as data behind figure). The blue circled bin at pulse center is individually significant (3.7σ); cyan circled points are at 2σ–3σ. The radio PAs (red) can be fit (excluding the circled point) with the normal mode (magenta) and orthogonal mode (red) i ∼ 60° models. For the i ∼ 120° model only the orthogonal mode solution is tenable. Note that the i ∼ 60° models better accommodate the late radio point and the X-ray data. A somewhat better match can be found for the orthogonal mode model when the X-ray emission is at higher altitude, with modest altitude h (dashed curve). Bottom: IXPE pulsar light curve (blue), Parkes 1.4 GHz light curve (red).(The data used to create this figure are available.)
Paper: The Polarized Cosmic Hand: IXPE Observations of PSR B1509−58/MSH 15−52 
Authors: Roger W. Romani, Josephine Wong, Niccoló Di Lalla, Nicola Omodei, Fei Xie, C.-Y. Ng, Riccardo Ferrazzoli, Alessandro Di Marco, Niccoló Bucciantini, Maura Pilia, Patrick Slane, Martin C. Weisskopf, Simon Johnston, Marta Burgay, Deng Wei, Yi-Jung Yang, Shumeng Zhang, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Nicoló Cibrario, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Ioannis Liodakis, Philip Kaaret, Vladimir Karas, Dawoon E. Kim, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Grzegorz Madejski, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Riccardo Middei, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Chiara Oppedisano, Luigi Pacciani, Alessandro Papitto, George G. Pavlov, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgró, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Silvia Zane
Figure caption: Morphological regions of interest on the IXPE combined DU1-3 2–8 keV image. The Hand’s “wrist” includes the bright jet and flanking filament structures, divided here into several regions.
Paper: The Polarized Cosmic Hand: IXPE Observations of PSR B1509−58/MSH 15−52 
Authors: Roger W. Romani, Josephine Wong, Niccoló Di Lalla, Nicola Omodei, Fei Xie, C.-Y. Ng, Riccardo Ferrazzoli, Alessandro Di Marco, Niccoló Bucciantini, Maura Pilia, Patrick Slane, Martin C. Weisskopf, Simon Johnston, Marta Burgay, Deng Wei, Yi-Jung Yang, Shumeng Zhang, Lucio A. Antonelli, Matteo Bachetti, Luca Baldini, Wayne H. Baumgartner, Ronaldo Bellazzini, Stefano Bianchi, Stephen D. Bongiorno, Raffaella Bonino, Alessandro Brez, Fiamma Capitanio, Simone Castellano, Elisabetta Cavazzuti, Chien-Ting Chen, Nicoló Cibrario, Stefano Ciprini, Enrico Costa, Alessandra De Rosa, Ettore Del Monte, Laura Di Gesu, Immacolata Donnarumma, Victor Doroshenko, Michal Dovčiak, Steven R. Ehlert, Teruaki Enoto, Yuri Evangelista, Sergio Fabiani, Javier A. Garcia, Shuichi Gunji, Kiyoshi Hayashida, Jeremy Heyl, Wataru Iwakiri, Ioannis Liodakis, Philip Kaaret, Vladimir Karas, Dawoon E. Kim, Takao Kitaguchi, Jeffery J. Kolodziejczak, Henric Krawczynski, Fabio La Monaca, Luca Latronico, Grzegorz Madejski, Simone Maldera, Alberto Manfreda, Frédéric Marin, Andrea Marinucci, Alan P. Marscher, Herman L. Marshall, Francesco Massaro, Giorgio Matt, Riccardo Middei, Ikuyuki Mitsuishi, Tsunefumi Mizuno, Fabio Muleri, Michela Negro, Stephen L. O'Dell, Chiara Oppedisano, Luigi Pacciani, Alessandro Papitto, George G. Pavlov, Matteo Perri, Melissa Pesce-Rollins, Pierre-Olivier Petrucci, Andrea Possenti, Juri Poutanen, Simonetta Puccetti, Brian D. Ramsey, John Rankin, Ajay Ratheesh, Oliver J. Roberts, Carmelo Sgró, Paolo Soffitta, Gloria Spandre, Douglas A. Swartz, Toru Tamagawa, Fabrizio Tavecchio, Roberto Taverna, Yuzuru Tawara, Allyn F. Tennant, Nicholas E. Thomas, Francesco Tombesi, Alessio Trois, Sergey Tsygankov, Roberto Turolla, Jacco Vink, Kinwah Wu, Silvia Zane
Figure caption: 2–5.5 keV polarization bars (orthogonal to the EVPA), as determined from simultaneous fitting inside the magenta region (cyan bars >4σ significance, green bars >3σ, white bars >2σ; the labels at upper right show the bar length for PD = 1). Here we employ a 15″ grid to better resolve the pulsar from inner nebula structures. Background is the full-band CXO image.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: History of gas kinematics, star formation, and MBH accretion for three low-mass dwarf galaxies between 108 < M star/M ⊙ < 108.3, with one star-forming dwarf (left) and two quiescent dwarfs (center+right). We trace the properties of the most massive MBH within 2 kpc of the halo center. Each column is labeled with the internal halo number from ROMULUS25. All panels except the top row include vertical lines marking t 90 (blue dotted for star-forming, red dotted for quiescent), as well as vertical lines marking mergers (dashed black; see Section 3.3 for details). 1st row: SFR (solid thick) and 103 × BHAR (solid thin) vs. cosmic time. 2nd row: sSFR for the target halo normalized to the median sSFR at the corresponding epoch, across star-forming galaxies between 108 < M star/M ⊙ < 108.3. 3rd row: Mass held within all gas particles (solid thick) and mass held within the H I component of gas particles (solid thin). 4th row: Ratio of energy in outflowing gas at 0.1 × R 200, to the energy required to escape the potential from 0.1 × R 200. For clarity, the horizontal line (solid thin) marks the 0.5 threshold. 5th row: Ratio of mass flux in outflowing gas to inflowing gas at 0.1 × R 200.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Left: total energy injection from MBHs and SNe as a function of the stellar mass for star-forming dwarfs with central MBHs (blue unfilled dots), quiescent dwarfs with central MBHs (red unfilled circles), and dwarfs entirely without MBHs (gray filled circles). Middle: fraction of energy injection contributed by MBHs as a function of the stellar mass for dwarfs with central MBHs. Quiescent dwarfs below M star/M ⊙ < 2 × 109 tend to have higher amounts of total energy injection at fixed stellar mass, and more of this energy injection tends to come from MBHs. Dwarfs above M star/M ⊙ > 2 × 109 have similar amounts of total energy injection, in line with simulation results from Pontzen et al. (2017). Only a small fraction of dwarfs are entirely dominated by energy injection from the MBH. Right: ﹩{M}_{\mathrm{BH}}^{\mathrm{acc}}\mbox{--}{M}_{\mathrm{star}}﹩ relation for quiescent and star-forming dwarfs with central MBHs. We fit the relation below M star/M ⊙ < 2 × 109 for quiescent galaxies (red solid) and star-forming galaxies (blue solid), showing the extrapolated fits with dashed lines.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Quiescent fraction across 25 sight lines as a function of the distance from the nearest massive neighbor. Legend is as in Figure 2. For comparison with Dickey et al. (2021), we distinguish between high-mass dwarfs (top panel, 109.5 < M star/M ⊙ < 1010) and low-mass dwarfs (bottom panel, 108.5 < M star/M ⊙ < 109). The black-shaded region indicates d host < 1.5 Mpc, the threshold for galaxy isolation. ROMULUS25 dwarfs (isolated and nonisolated) exhibit the same trends as most other simulations, showing quiescent fractions in agreement with observations for high-mass dwarfs, but predicting too many quiescent low-mass dwarfs. At low masses, all simulations produce too many quiescent dwarfs even within group environments with d host < 1.5 Mpc.
Paper: Active Galactic Nucleus Quenching in Simulated Dwarf Galaxies
Authors: Ray S. Sharma, Alyson M. Brooks, Michael Tremmel, Jillian Bellovary, Thomas R. Quinn
Figure caption: Quiescent fraction across 25 sight lines in ROMULUS25 as a function of the distance from the nearest massive neighbor, distinguishing between all dwarfs (blue), those with central MBHs (yellow), and those with no MBH (purple). As in Figure 7, we distinguish between high-mass dwarfs (top panel, 109.5 < M star/M ⊙ < 1010) and low-mass dwarfs (bottom panel, 108.5 < M star/M ⊙ < 109). Uncertainties are omitted on the “All” line for clarity. The gray-shaded region marks d host < 1.5 Mpc, the threshold for galaxy isolation. High-mass dwarfs with central MBHs are equally likely to be quenched in the field relative to those without MBHs. Low-mass ROMULUS25 dwarfs with central MBHs are more likely to be quenched in both the field and in groups, relative to those without MBHs. Dwarfs without MBHs in both mass ranges show closer agreement to observations of the quiescent fraction (Dickey et al. 2021, black squares).