adsabs/AstroCLIMB huggingface dataset:
Paper: A CHIME/FRB Study of Burst Rate and Morphological Evolution of the Periodically Repeating FRB 20180916B
Authors: Ketan R. Sand, Daniela Breitman, Daniele Michilli, Victoria M. Kaspi, Pragya Chawla, Emmanuel Fonseca, Ryan Mckinven, Kenzie Nimmo, Ziggy Pleunis, Kaitlyn Shin, Bridget C. Andersen, Mohit Bhardwaj, P. J. Boyle, Charanjot Brar, Tomas Cassanelli, Amanda M. Cook, Alice P. Curtin, Fengqiu Adam Dong, Gwendolyn M. Eadie, B. M. Gaensler, Jane Kaczmarek, Adam Lanman, Calvin Leung, Kiyoshi W. Masui, Mubdi Rahman, Ayush Pandhi, Aaron B. Pearlman, Emily Petroff, Masoud Rafiei-Ravandi, Paul Scholz, Vishwangi Shah, Kendrick Smith, Ingrid Stairs, David C. Stenning
Figure caption: Flowchart showing the Baseband Morphology Pipeline. The path on the left involves extracting the Stokes intensity (I) data products from the beamformed file, dedispersing and cleaning the spectra, getting the burst profile and estimating the number of subbursts/peaks to fit for. The middle portion indicates the process of extracting initial guesses on the temporal profile of each subburst, first by a least-squares (LS) fit and then by Markov Chain Monte Carlo (MCMC) sampling using an exponential modified Gaussian (EMG). As indicated in the right-hand column we then estimate the spectral parameters using the same methods assuming a running power-law (RPL) model. The resulting data file along with initial guesses are then provided to fitburst.
Paper: A Universal Equation to Predict Ωm from Halo and Galaxy Catalogs
Authors: Helen Shao, Natalí S. M. de Santi, Francisco Villaescusa-Navarro, Romain Teyssier, Yueying Ni, Daniel Anglés-Alcázar, Shy Genel, Ulrich P. Steinwandel, Elena Hernández-Martínez, Klaus Dolag, Christopher C. Lovell, Lehman H. Garrison, Eli Visbal, Mihir Kulkarni, Lars Hernquist, Tiago Castro, Mark Vogelsberger
Figure caption: Top: we quantify the behavior of the analytic expressions, discussed in Section 4.2, in the presence of supersample covariance. We test the analytic expressions on 100 ﹩{(25\,{h}^{-1}\,\mathrm{Mpc}))}^{3}﹩ subvolumes randomly selected from the IllustrisTNG-300 simulation without imposing periodic boundary conditions. The simulation contains a total volume of ﹩{(205\,{h}^{-1}\,\mathrm{Mpc}))}^{3}﹩ and was run with a cosmology of Ωm = 0.308. The plots depict the difference between the true Ω value and the predicted for the galaxy catalogs constructed using each of the four stellar mass thresholds as indicated at the top of each column. For all catalogs, the predictions are corrected for their negative offset from the truth by introducing a bias in the analytic expression for the final MLP, b = − 0.19, which shifts all predictions upwards by a constant. After adjusting for this common offset, the predictions exhibit mean relative errors of ∼11.1%, comparable to the predictions for galaxy catalogs from other hydrodynamic simulation codes as discussed in Section 4.2.2. The common offset can be attributed to the fact that the equations were trained only on simulation volumes of ﹩{(25\,{h}^{-1}\,\mathrm{Mpc})}^{3}﹩ with periodic boundary conditions and are now being tested on simulations without such conditions. We confirm this reasoning with the results shown in the bottom panel. Bottom: this panel follows the same format as the one above. We show that the analytic equations behave similarly when evaluated on 27 IllustrisTNG simulations from the CV set (see Section 2) after removing periodic boundary conditions. These simulations were run with the same cosmology Ωm = 0.308. All predictions for galaxy catalogs constructed from these simulations possess a negative offset equal to the one found for the predictions from IllustrisTNG-300 subvolumes, which was adjusted for by introducing a bias to the final MLP equation: b = − 0.19. After doing so, the predictions exhibit only a mean relative error of ∼2.2%. These results indicate that the analytic equations are able to account for the effects of supersample covariance if one simply shifts the predictions by a constant bias, b, due to the presence of periodic boundary conditions in the training data.
Paper: A Universal Equation to Predict Ωm from Halo and Galaxy Catalogs
Authors: Helen Shao, Natalí S. M. de Santi, Francisco Villaescusa-Navarro, Romain Teyssier, Yueying Ni, Daniel Anglés-Alcázar, Shy Genel, Ulrich P. Steinwandel, Elena Hernández-Martínez, Klaus Dolag, Christopher C. Lovell, Lehman H. Garrison, Eli Visbal, Mihir Kulkarni, Lars Hernquist, Tiago Castro, Mark Vogelsberger
Figure caption: This plot shows the predictions of the original equations found by the symbolic regression algorithm evaluated on the halo catalogs of the Gadget test set. As can be seen, while it achieves similar accuracy to the GNN model, with a mean relative error of 7.1%, it is not as accurate as the modified expressions, which had an error of 6.6%. See Figure 2.
Paper: A Universal Equation to Predict Ωm from Halo and Galaxy Catalogs
Authors: Helen Shao, Natalí S. M. de Santi, Francisco Villaescusa-Navarro, Romain Teyssier, Yueying Ni, Daniel Anglés-Alcázar, Shy Genel, Ulrich P. Steinwandel, Elena Hernández-Martínez, Klaus Dolag, Christopher C. Lovell, Lehman H. Garrison, Eli Visbal, Mihir Kulkarni, Lars Hernquist, Tiago Castro, Mark Vogelsberger
Figure caption: We evaluate the analytic equations discussed in Section 4.2 on galaxy catalogs from the SWIFT-EAGLE simulation set constructed using four different minimum stellar mass thresholds: N × m * for N ∈ {3, 4, 5, 6} where m * is a fixed mass for a single stellar particle. Each column is labeled with the corresponding mass cut. We note that, since the SWIFT-EAGLE simulations were generated using the same initial random seed, there is a high correlation between the galaxy catalogs of the different stellar mass thresholds for this simulation set that is responsible for the trend of decreasing accuracy as the stellar mass threshold increases.
Paper: A Universal Equation to Predict Ωm from Halo and Galaxy Catalogs
Authors: Helen Shao, Natalí S. M. de Santi, Francisco Villaescusa-Navarro, Romain Teyssier, Yueying Ni, Daniel Anglés-Alcázar, Shy Genel, Ulrich P. Steinwandel, Elena Hernández-Martínez, Klaus Dolag, Christopher C. Lovell, Lehman H. Garrison, Eli Visbal, Mihir Kulkarni, Lars Hernquist, Tiago Castro, Mark Vogelsberger
Figure caption: We evaluate the analytic equations discussed in Section 4.2 on galaxy catalogs from the Astrid simulation set constructed using four different minimum stellar mass thresholds: N × m * for N ∈ {3, 4, 5, 6} where m * is a fixed mass for a single stellar particle. Each column is labeled with the corresponding mass cut. As it can be seen, the accuracies of the equations are preserved for the different mass thresholds demonstrating that the model has marginalized over the number density of galaxies.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The atlas of five H I-resolved galaxies (see also Appendix B). RPS and TS galaxies are plotted on the left and right, respectively. For each galaxy, the DECaLS DR9 optical image and the WALLABY H I-column-density map are placed adjacently. In the H I intensity map, only pixels with values >5σ are shown. The optical image is overlaid with the contour of N H I , with levels of 1, 2, 4, and 8 × 1020 cm−1. The lowest and the highest level are plotted as dotted and dashed lines, respectively, for clarity. The ID, beam size (∼30″), 5 kpc scale bar, stellar mass, and the relevant values of f and S are given at each panel. The direction of the group center is indicated by a cyan arrow for RPS galaxies, with the direction of the major tidal perturber by a magenta arrow for TS ones.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The influence of model specification on the values of t str and t dpl. Panels are similar to Figures 13(a) and (b). Four models are plotted with different line-styles and patches. The main model we used is the solid red line. For details of other three models, please refer to the text. In panel (b) the criterion of gas depletion is reaching 1.06 dex below the mean M H I –M * relation.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The same as Figure 7, but only H I-detected high-mass galaxies are plotted. The bisector fitting results of Figure 7 are plotted as references. The x-axis range is the same as that in Figure 7.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Comparing our MSS stars to the gaseous MS measurements from Nidever et al. (2010), in the transverse stream coordinate B MS (top) and the LSR-corrected radial velocity (bottom). The log-scaled H I column density of the MS is shown in gray, with our MSS candidates overlaid and colored by stellar metallicity. The point size is inversely proportional to the heliocentric distance. The dotted blue line indicates the approximate extent of the ionized H II MS as measured by Fox et al. (2014). Overlaid in blue (orange) is the predicted track of stripped MSS stars from Model 1 (Model 2) in Besla et al. (2012). For the LMC and SMC colors we use median metallicities of −0.5 and −1.0, respectively, noting that they both have significant spreads in metallicity (Hasselquist et al. 2021). Arrows in the top panel denote the proper motion of the MSS stars and the Clouds, scaled to 50 Myr of motion. Note that these axes are horizontally flipped compared to the convention of Nidever et al. (2010), in order to match the orientation of the Galactic maps elsewhere in this work.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Selecting stars associated with the Clouds in angular momentum space. The left panels show predictions from existing data and simulations. Gray contours indicate the 3σ distribution of stars beyond 50 kpc in the smooth mock halo of Robin et al. (2012). We show simulation particles beyond 30 kpc of the three largest contributors to the outer halo: the Clouds and MSS (Besla et al. 2012, 2013; blue and orange), the Sagittarius Stream (Vasiliev et al. 2021; green), and the GSE merger (Naidu et al. 2021; pink). Black stars indicate the observed mean angular momenta of the Clouds. The right panels show data from our MagE survey beyond 50 kpc, along with the corresponding red (blue) selection made in the L X (L Y) space. The combination of L X−L Y−L Z cuts isolates stars moving with the Clouds.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Selection of the MSS from our survey data. Top: 191 stars beyond 50 kpc in angular momentum space, with our kinematically selected MSS stars colored by metallicity. The MSS stands out as a prominent tail of stars with highly negative L X, and we select stars within 1σ  of the adopted L X selection boundary. Bottom: H I column density of the MS, with our identified MSS stars overlaid. The dashed lines trace the past 500 Myr orbit of the Clouds (Patel et al. 2020).
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Spectroscopic distances for our identified MSS stars as a function of MS longitude. Shaded bands contain 90% of the trailing tidal stellar debris from the simulations of Besla et al. (2012). The dashed black line indicates the linear fit to the observed distance gradient along the MSS, along with a 1σ shaded region.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Kinematically selected MSS stars in chemical abundance space, colored by metallicity as throughout this work. Median tracks for the LMC, SMC, and GSE dwarf galaxies are overlaid (Hasselquist et al. 2021).
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Validating the spectroscopic distance scale of our survey with stars from the Sextans and Crater 2 dwarf galaxies. We recover literature distances within 1σ in the mean, and the statistical distance uncertainties are well calibrated.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Results from our Monte Carlo trials to determine which stars in our >50 kpc sample have orbits that plausibly lead back to the Clouds (see text for details). Orbits are integrated backward for 6 Gyr in the MW+LMC+SMC potential. The horizontal axis shows the long-term (older than 0.5 Gyr) orbital pericenter relative to the LMC, with error bars denoting the 16th and 84th quantiles. The vertical axis shows the fraction of Monte Carlo trials in which the star remains bound to the LMC, quantified by the presence of a pericenter >2 Gyr ago within the LMC tidal radius of 60 kpc.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: The emerging picture of the MW’s outer halo. The color map shows the density distribution of RGB stars beyond >50 kpc from the Gaia XP catalog of Chandra et al. (2023), smoothed with a 5° beam. We highlight the prominent overdensities that dominate the outer halo, as well as their most plausible progenitors. The Sagittarius Stream was first extensively mapped by Majewski et al. (2003), and the outer Virgo 0verdensity (Sesar et al. 2017) and Pisces overdensity (Sesar et al. 2007) were argued by Chandra et al. (2023) to be distant imprints of the GSE merger. The elongated Pisces Plume was previously identified as the dynamical friction wake of the LMC (Belokurov et al. 2019; Conroy et al. 2021). In this work, we have found a substantial population of MSS stars that overlap with the Pisces Plume.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Projection of our MSS stars along the L MS coordinate, against B MS (panel 1), heliocentric distance (panel 2), Galactocentric radial velocity (panel 3), and proper motions along and transverse to the MS (panels 4 and 5). Particles from both tidal debris models in Besla et al. (2012) are shown, along with the Clouds-associated debris from the H3 Survey presented by Z20.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Integrated past orbits for our sample of MSS stars, in a rigid time-varying potential with LMC and SMC contributions adopted from Patel et al. (2020). The top left panel shows orbits for the past gigayear in Galactic coordinates, and the bottom left panel shows the same in the Galactocentric Y-Z plane. The top (bottom) right panel shows distances with respect to the MW (LMC) center of mass over 6 Gyr, for both our MSS stars and the entire >50 kpc giant sample from our survey. These panels only show orbits computed with mean phase-space positions, so several stars “unbound” to the LMC here have a nonzero probability of becoming bound in our orbital simulations (see Figure 9).
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: Integrated mass in the neutral MS gas, for a fixed distance of 55 kpc (black) and with our measured distance gradient for the stellar stream (red). The shaded band encompasses the 1σ uncertainty on our distance gradient.
Paper: Discovery of the Magellanic Stellar Stream Out to 100 kpc
Authors: Vedant Chandra, Rohan P. Naidu, Charlie Conroy, Ana Bonaca, Dennis Zaritsky, Phillip A. Cargile, Nelson Caldwell, Benjamin D. Johnson, Jiwon Jesse Han, Yuan-Sen Ting, 源森 丁
Figure caption: A segment of our MagE spectra for the MSS stars presented in this work, with the data shown in black and the fitted MINESweeper model shown in red. Spectra have been shifted to the rest frame.
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: Comparison of the fractions of gas strippable by ram pressure (f RPS) and by tidal interaction (f tid). (a) How the strippable gas fraction f str changes with the projected distance d proj from the center of N4636G. If a galaxy has both f RPS (blue-edged slashed) and f tid (orange-edged backslashed) positive, the larger one is plotted as a circle, with the other plotted as a translucent dot. These two symbols are connected with a gray dotted thin line. The circle, color-coded by Δlog M H I , has a radius related to the stellar mass. Thus, the blue-edged circles and orange-edged circles correspond to the RPS and TS sample, respectively. (b) Distributions of the f RPS of the RPS sample (blue slashes) and the f tid of the TS sample (orange backslashes). The positive f RPS of the TS sample (translucent blue patch) and the positive f tid of the RPS sample (translucent orange patch) are stacked as well. The results of K-S tests between f RPS and f tid, either limited to the RPS and TS samples or including all nonzero values, are given. An orange dashed line is drawn at the median value of f tid. (c) Fitting result of f RPS using Equation (10). Galaxies are divided (and color-coded) into four bins according to Δlog M H I , and the four corresponding fitted lines are plotted as dashed lines of respective colors. Squares (and circles) are gas-poor (gas-rich) galaxies. (d) Fitting result of f str. The symbols are the same as in panel (c).
Paper: FAST-ASKAP Synergy: Quantifying Coexistent Tidal and Ram Pressure Strippings in the NGC 4636 Group
Authors: Xuchen Lin, 旭辰 林, Jing Wang, 菁 王, Virginia Kilborn, Eric W. Peng, Luca Cortese, Alessandro Boselli, Ze-Zhong Liang, 泽众 梁, Bumhyun Lee, Dong Yang, 冬 杨, Barbara Catinella, N. Deg, H. Dénes, Ahmed Elagali, P. Kamphuis, B. S. Koribalski, K. Lee-Waddell, Jonghwan Rhee, Li Shao, 立 邵, Kristine Spekkens, Lister Staveley-Smith, T. Westmeier, O. Ivy Wong, Kenji Bekki, Albert Bosma, Min Du, 敏 杜, Luis C. Ho, Juan P. Madrid, Lourdes Verdes-Montenegro, Huiyuan Wang, 慧元 王, Shun Wang, 舜 王
Figure caption: The evolution of galaxies’ Δlog M H I  as they infall. Only galaxies with an sSFR > 10−11 yr−1 are plotted in this figure. H I detections (circle) and nondetections (semicircle, plotted using the upper limit) are color-coded by Δlog SFR. The radius of these circles and semicircles correlates with the stellar mass. The medians of d proj and the 95th percentiles of Δlog M H I  (including H I nondetections but not low-sSFR galaxies) in five even d proj bins are given in orange, and the uncertainties are estimated with bootstrap. Hypothetical evolutionary paths for infalling galaxies with different initial Δlog M H I  are plotted as green dashed–dotted lines. The Spearman rank correlation and the p-value are given. The galaxy pair are indicated by cyan-edged triangles. The line of f str = 100% is plotted as green dotted lines, above which galaxies should not appear in our model. The evolutionary path with star formation as the only gas consumption is plotted with gray lines for reference.