The First Galaxies and the Likely Discovery of Their Fossils in the Local Group by Massimo Ricotti

“…It is widely believed that reionization stopped star formation in fossil dwarfs. However, here we dispute this idea and discuss a physical mechanism whereby recent episodes of star formation would be produced in some fossil dwarfs that, hence, may characterized by a bimodal star formation history. …”
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The Arizona Molecular ISM Survey with the SMT: Variations in the CO(2–1)/CO(1–0) Line Ratio across the Galaxy Population by Ryan P. Keenan, Daniel P. Marrone, Garrett K. Keating

“…We find strong trends between r _21 and SFR, SFR surface density, star formation efficiency, and distance from the star formation main sequence (SFMS). …”
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The Prevalence of Star-forming Clumps as a Function of Environmental Overdensity in Local Galaxies by Dominic Adams, Hugh Dickinson, Lucy Fortson, Kameswara Mantha, Vihang Mehta, Jürgen Popp, Claudia Scarlata, Chris Lintott, Brooke Simmons, Mike Walmsley

“…At the peak of cosmic star formation (1 ≲ z ≲ 2), the majority of star-forming galaxies hosted compact, star-forming clumps, which were responsible for a large fraction of cosmic star formation. …”
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Galaxy Evolution in a Pilot Survey up to z=1 and CDM Halos by E. Giraud, J. Melnick, Q.-S. Gu, H. Quintana, F. Selman, I. Toledo, P. Zelaya

“…Our observations indicate that at z⩽1 star formation and hierarchical structure formation of CDM halos are not in phase.…”
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Improved SED-fitting Assumptions Result in Inside-out Quenching at z ~ 0.5 and Quenching at All Radii Simultaneously at z ~ 1 by Alexander de la Vega, Susan A. Kassin, Camilla Pacifici, Stéphane Charlot, Emma Curtis-Lake, Jacopo Chevallard, Timothy M. Heckman, Anton M. Koekemoer, Weichen Wang

“…Many studies conclude that galaxies quench from the inside-out by examining profiles of specific star formation rate (sSFR). These are usually measured by fitting spectral energy distributions (SEDs) assuming a fixed dust law and uniform priors on all parameters. …”
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Multiepoch Observations of the Nearby Spiral Galaxy NGC 3938 with the Chandra X-Ray Observatory by Siddhi Raut, Eric M. Schlegel, Thomas G. Pannuti, Brannon W. Jones, Jacobo Matallana

“…The luminosity function of NGC 3938 is compared to a recent compilation of 38 galaxies, and we identify a potentially significant problem with the “known” distance to NGC 3938. Star formation rate and metallicity values are also computed; the star formation rate is highly dependent on the adopted distance. …”
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Deep Swift/UVOT Observations of GOODS-N and the Evolution of the Ultraviolet Luminosity Function at 0.2 < z < 1.2 by Alexander Belles, Caryl Gronwall, Michael H. Siegel, Robin Ciardullo, Mat J. Page

“…From the LF fits in various redshift bins, we calculate the star formation rate density as a function of redshift and find evolution consistent with past works. …”
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Exploring the Evolution of a Dwarf Spheroidal Galaxy with SPH Simulations. II. AGN Feedback by Roberto Hazenfratz, Paramita Barai, Gustavo A. Lanfranchi, Anderson Caproni

“…While AGN feedback is generally negative on star formation, instances of positive feedback were also identified. …”
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AEOS: Transport of Metals from Minihalos following Population III Stellar Feedback by Jennifer Mead, Kaley Brauer, Greg L. Bryan, Mordecai-Mark Mac Low, Alexander P. Ji, John H. Wise, Andrew Emerick, Eric P. Andersson, Anna Frebel, Benoit Côté

“…The loss of metals to regions well beyond the virial radius delays the onset of enriched star formation and extends the period that Population III star formation can persist. …”
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Evidence for AGN Feedback in Galaxy Clusters and Groups by Myriam Gitti, Fabrizio Brighenti, Brian R. McNamara

“…Understanding the physics of the hot gas and its interplay with the relativistic plasma ejected by the AGN is key for understanding the growth and evolution of galaxies and their central black holes, the history of star formation, and the formation of large-scale structures. …”
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A Principle Component Analysis of Galaxy Properties from a Large, Gas-Selected Sample by Yu-Yen Chang, Rikon Chao, Wei-Hao Wang, Pisin Chen

“…In addition, the near-infrared color (i-J) shows an obvious second principal component that might provide evidence of the complex old star formation. Based on our data, we suggest that it is premature to pronounce the failure of the CDM model and it motivates more theoretical work.…”
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Cluster Candidates with Massive Quiescent Galaxies at z ∼ 2 by Tomokazu Kiyota, Makoto Ando, Masayuki Tanaka, Alexis Finoguenov, Sadman Shariar Ali, Jean Coupon, Guillaume Desprez, Stephen Gwyn, Marcin Sawicki, Rhythm Shimakawa

“…There is no clear evidence of enhancement nor suppression of the star formation rate of the main-sequence galaxies in the clusters. …”
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Overview of the Near-IR S0 Galaxy Survey (NIRS0S) by E. Laurikainen, H. Salo, R. Buta, J. H. Knapen

“…It was estimated that the spiral bulges brighter than −20 mag in K-band are massive enough to be converted into the bulges of S0s merely by star formation. Bars were found to be fairly robust both in S0s and spirals, but, inspite of that, bars might evolve significantly within the Hubble sequence.…”
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Complex Structure around a Circumstellar Disk Caused by Interchange Instability by Masahiro N. Machida, Shantanu Basu

“…The structures extend to >1000 au and persist for at least 30,000 yr after protostar formation, demonstrating the dynamic removal process of magnetic flux during star formation. We find that the disk continues to grow even as interchange instability occurs, by accretion through channels between the outgoing cavities. …”
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The Low-Mass End of the MBH/Mhost Relation in Quasars by Roberto Decarli, Renato Falomo, Jari K. Kotilainen, Tomi Hyvönen, Michela Uslenghi, Aldo Treves

“…Host galaxy luminosities and stellar masses are computed, under reasonable assumptions on their star formation histories. Combining these results with those from our previous studies, we manage to extend the sampled parameter space of the MBH-Mhost relation in quasars. …”
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On the Formation of Planets in the Milky Way’s Thick Disk by Tim Hallatt, Eve J. Lee

“…One key difference between the two stellar populations is the time at which they emerged: thick-disk stars are the likely product of cosmic noon (redshift z ∼ 2), an era characterized by high star formation rate, massive and dense molecular clouds, and strong supersonic turbulence. …”
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Mapping the Active Galactic Nucleus Effects on the Stellar and Gas Properties of NGC 5806 by Sophie L. Robbins, Sandra I. Raimundo, Matthew A. Malkan

“…We use emission line ratios to map gas metallicity and identify regions of gas excitation dominated by AGN/shocks or star formation. We also determine the average stellar population age and metallicity, and model the rotation and dynamics of the galaxy. …”
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FEASTS: Radial Distribution of H i Surface Densities Down to 0.01 M⊙ pc−2 of 35 Nearby Galaxies by Jing Wang, Dong Yang, Xuchen Lin, Qifeng Huang, Zhijie Qu, Hsiao-wen Chen, Hong Guo, Luis C. Ho, Peng Jiang, Zezhong Liang, Céline Péroux, Lister Staveley-Smith, Simon Weng

“…Excluding strongly tidal-interacting galaxies, the ratio R _001 / R _1 (anti)correlates strongly and significantly with the H i -to-stellar mass ratio and specific star formation rate, but not with the stellar mass, M _H _i , dark matter mass, or star formation rate. …”
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What Drives the H i Content of Central Galaxies—A Comparison between Hydrodynamic Simulations and Observations Using Random Forest by Xiao Li, Cheng Li, H. J. Mo

“…Beyond that, the accretion rate of supermassive black holes is the most important feature in TNG, while specific star formation rate is the top ranked in EAGLE. This result can be understood from the fact that the H i gas is regulated mainly by thermal-mode AGN feedback in TNG and by stellar feedback in EAGLE. …”
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CH3OH Thermal Lines Traces 6.7 GHz CH3OH Maser Variation of High-mass Protostar G353.273+0.641 by Shi-Min Song, Xi Chen, Sheng-Yuan Liu, Jun-Ting Liu

“…These results emphasize the significance of integrating the variations in 6.7 GHz CH _3 OH masers with their surrounding circumstellar environments to advance our comprehension of high-mass star formation mechanisms.…”
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