Constraints on the Cosmological Coupling of Black Holes from the Globular Cluster NGC 3201 by Carl L. Rodriguez

“…Globular clusters are among the oldest stellar populations in the Milky Way; consequently, they also host some of the oldest known stellar-mass black holes, providing insight into black hole formation and evolution in the early ( z ≳ 2) universe. …”
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Galaxy Modelling -- I. Spectral Energy Distributions from Far-UV to Sub-mm Wavelengths by Devriendt, J, Guiderdoni, B, Sadat, R

“…In order to derive the SEDs in this broad spectral range, we first couple spectrophotometric and (closed-box) chemical evolutions to account for metallicity effects on the spectra of synthetic stellar populations. We then use a phenomenological fit for the metal-dependent extinction curve and a simple geometric distribution of the dust to compute the optical depth of galaxies and the corresponding obscuration curve. …”

ACS photometry of extended, luminous globular clusters in the outskirts of M31 by Mackey, A, Huxor, A, Ferguson, AMN, Tanvir, N, Irwin, M, Ibata, R, Bridges, T, Johnson, R, Lewis, G

“…Our F606W, F814W color-magnitude diagrams extend ∼3 mag below the horizontal branch level, and clearly demonstrate, for the first time, that all four clusters are composed of ≳ Gyr old, metal-poor stellar populations. No evidence for multiple populations is observed. …”

Clustering of supernova ia host galaxies by Carlberg, R, Sullivan, M, Le Borgne, D, Conley, A, Howell, D, Perrett, K, Astier, P, Balam, D, Balland, C, Basa, S, Hardin, D, Fouchez, D, Guy, J, Hook, I, Pain, R, Pritchet, C, Regnault, N, Rich, J, Perlmutter, S

“…We conclude that these supernova clustering differences are primarily the expected outcome of the dependence of supernova rates on galaxy masses and stellar populations with their clustering environment. © 2008. …”

Hierarchical models of high redshift galaxies with thermally pulsing asymptotic giant branch stars: comparison with observations by Tonini, C, Maraston, C, Thomas, D, Devriendt, J, Silk, J

“…This indicates that the AGN feedback recipe that is adopted to regulate the high-mass end of the luminosity function should be sophisticated to take the effect of the stellar populations into account at high redshifts.…”

Chemical evolution with radial mixing by Schönrich, R, Binney, J

“…Radial mixing of stellar populations with high σ _z with age than predicted by theory. …”

Testing the limit of AO for ELTs: Diffraction limited astronomy in the red optical by Tecza, M, Magorrian, J, Thatte, N, Clarke, F

“…Prominent ELT science cases that use the Calcium triplet can exploit this gain in spatial resolution in the red-optical: stellar populations in dense environments or crowded fields; and the case of intermediate mass black holes in nuclear and globular stellar clusters, as well as (super-) massive black holes in galaxies.…”

SAURON: integral-field spectroscopy of galaxies by Peletier, R, Davies, R, Allington-Smith, JR, Bacon, R, Copin, Y, Emsellem, E, de Zeeuw, P, Miller, B, Bureau, M, Verolme, E, Carollo, C, Monnet, G

“…In combination with available long-slit spectroscopy of the outer regions of the galaxies, HST spectra of the nuclei, and HST imaging, we will constrain the intrinsic shapes, mass-to-light ratios, and stellar populations in spheroids. In this presentation we will give a status report and preliminary results from our first science run in February 1999. © Elsevier Science B.V.…”

The Dusty Red Supergiant Progenitor and the Local Environment of the Type II SN 2023ixf in M101 by Zexi Niu, Ning-Chen Sun, Justyn R. Maund, Yu Zhang, Ruining Zhao, Jifeng Liu

“…We also derived the star formation history of the SN environment based on resolved stellar populations, and the most recent star-forming epoch corresponds to a progenitor initial mass of 17–19 M _⊙ , in agreement with that from our SED fitting. …”
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A Semi-analytical Model for Stellar Evolution in AGN Disks by Alexander J. Dittmann, Matteo Cantiello

“…This model will enable more detailed studies of stellar populations and their interaction with accretion disks than have previously been possible.…”
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A Comprehensive Catalog of Emission-line Nebulae, Star Clusters, and Supergiants in M31 from the LAMOST Spectroscopic Survey by Pinjian Chen, Bingqiu Chen, Xuan Fang, Haibo Yuan, Baisong Zhang, Xiangwei Zhang, Jiarui Sun, Xiaowei Liu

“…Spectroscopic observations of various tracers in nearby galaxies, such as Andromeda (M31), play a crucial role in identifying and classifying individual stellar populations and nebular objects, thereby enhancing our understanding of galactic composition, environment, and dynamics, as well as stellar evolution. …”
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Light-curve Recovery with the Vera Rubin Observatory’s LSST. I. Pulsating Stars in Local Group Dwarf Galaxies by M. Di Criscienzo, S. Leccia, V. Braga, I. Musella, G. Bono, M. Dall’Ora, G. Fiorentino, M. Marconi, R. Molinaro, V. Ripepi, K. Carrell, Y. Choi, S. Savarese, L. Schreiber

“…We show that this exercise is essential to understand the potential of LSST in this field since excellent recovery is necessary to optimize the use of predicted period–luminosity, period–amplitude, and color–color relations to constrain the cosmic distance scale and the metallicity distribution function of different stellar populations.…”
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UGC 7639: A Dwarf Galaxy in the Canes Venatici I Cloud by L. M. Buson, D. Bettoni, P. Mazzei, G. Galletta

“…Ultraviolet images show that UGC 7639 inner regions are composed mostly by young stellar populations. In addition, we used smoothed particle hydrodynamics simulations with chemophotometric implementation to account for its formation and evolution. …”
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The Star Formation History of Nearby Galaxies: A Machine Learning Approach by Yujiao Yang, Chao Liu, Ming Yang, Yun Zheng, Hao Tian

“…In this study, we refine the synthetic CMD method with a state-of-the-art theoretical stellar evolution model to simulate the properties of stellar populations, incorporate the convolutional neural network in the fitting process to enhance the efficiency, and innovate the initial stellar mass estimation to improve the flexibility. …”
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Rejuvenated Accretors Have Less Bound Envelopes: Impact of Roche Lobe Overflow on Subsequent Common Envelope Events by M. Renzo, E. Zapartas, S. Justham, K. Breivik, M. Lau, R. Farmer, M. Cantiello, B. D. Metzger

“…Despite their high mass, our accretors also experience extended “blue loops,” which may have observational consequences for low-metallicity stellar populations and asteroseismology.…”
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Age dating of an early Milky Way merger via asteroseismology of the naked-eye star ν Indi by Chaplin, William J., Serenelli, Aldo M., Miglio, Andrea, Morel, Thierry, Mackereth, J. Ted, Vincenzo, Fiorenzo, Kjeldsen, Hans, Basu, Sarbani, Ball, Warrick H., Stokholm, Amalie, Verma, Kuldeep, Mosumgaard, Jakob Rørsted, Silva Aguirre, Victor, Mazumdar, Anwesh, Ranadive, Pritesh, Antia, H. M., Lebreton, Yveline, Ong, Joel, Appourchaux, Thierry, Bedding, Timothy R., Christensen-Dalsgaard, Jørgen, Creevey, Orlagh, García, Rafael A., Handberg, Rasmus, Huber, Daniel, Kawaler, Steven D., Lund, Mikkel N., Metcalfe, Travis S., Stassun, Keivan G., Bazot, Michäel, Beck, Paul G., Bell, Keaton J., Bergemann, Maria, Buzasi, Derek L., Benomar, Othman, Bossini, Diego, Bugnet, Lisa, Campante, Tiago L., Orhan, Zeynep Çelik, Corsaro, Enrico, González-Cuesta, Lucía, Davies, Guy R., Di Mauro, Maria Pia, Egeland, Ricky, Elsworth, Yvonne P., Gaulme, Patrick, Ghasemi, Hamed, Guo, Zhao, Hall, Oliver J., Hasanzadeh, Amir, Hekker, Saskia, Howe, Rachel, Jenkins, Jon M., Jiménez, Antonio, Kiefer, René, Kuszlewicz, James S., Kallinger, Thomas, Latham, David W., Lundkvist, Mia S., Mathur, Savita, Montalbán, Josefina, Mosser, Benoit, Bedón, Andres Moya, Nielsen, Martin Bo, Örtel, Sibel, Rendle, Ben M., Ricker, George R., Rodrigues, Thaíse S., Roxburgh, Ian W., Safari, Hossein, Schofield, Mathew, Seager, Sara, Smalley, Barry, Stello, Dennis, Szabó, Róbert, Tayar, Jamie, Themeßl, Nathalie, Thomas, Alexandra E. L., Vanderspek, Roland K., van Rossem, Walter E., Vrard, Mathieu, Weiss, Achim, White, Timothy R., Winn, Joshua N., Yıldız, Mutlu

“…Although these accreted stellar populations can be forensically identified as kinematically distinct structures within the Galaxy, it is difficult in general to date precisely the age at which any one merger occurred. …”
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The evolution of the Fundamental Plane of radio galaxies from z~0.5 to the present day by Herbert, P, Jarvis, M, Willott, C, McLure, R, Mitchell, E, Rawlings, S, Hill, G, Dunlop, J

“…We find that the low-luminosity, FRI-type, radio galaxies in our sample are consistent with the local Fundamental Plane of radio galaxies defined by Bettoni et al. when corrected for simple passive evolution of their stellar populations. However, we find that the higher luminosity, FRII-type radio galaxies are inconsistent with the local Fundamental Plane if only passive evolution is considered, and find evidence for a rotation in the Fundamental Plane at z~0.5 when compared with the local relation. …”

Dual effects of ram pressure on star formation in multiphase disk galaxies with strong stellar feedback by Lee, J, Kimm, T, Katz, H, Rosdahl, J, Devriendt, J, Slyz, A

“…Dense gas clumps with n H gsim 10 M ⊙ pc−2 are easily identified in extraplanar regions, but no significant young stellar populations are found in such clumps. In our attempts to enhance radiative cooling by adopting a colder ICM of T = 106 K, only a few additional stars are formed in the tail region, even if the amount of newly cooled gas increases by an order of magnitude.…”

Chemical evolution with radial mixing by Schönrich, R, Binney, J

“…Radial mixing of stellar populations with high σz from inner regions of the disc to the solar neighbourhood provides a natural explanation of why measurements yield a steeper increase of σz with age than predicted by theory. …”

Star formation in nearby early-type galaxies: Mapping in UV, optical and CO by Bureau, M, Bacon, R, Cappellari, M, Combes, F, Davies, R, De Zeeuw, P, Emsellem, E, Falcn-Barroso, J, Jeong, H, Krajnovi, D, Kuntschner, H, McDermid, R, Peletier, R, Sarzi, M, Shapiro, K, Van De Ven, G, Yi, S, Young, L

“…CO also traces well the young stellar populations and ionised gas distribution and kinematics, but in KDCs not always the stellar kinematics Emsellem et al. 2004; Sarzi et al. 2006; Kuntschner et al. 2006). © 2007 International Astronomical Union.…”