Zobrazeno 1 - 10
of 351
pro vyhledávání: '"Christensen, Charlotte"'
Autor:
Riggs, Claire L., Brooks, Alyson M., Munshi, Ferah, Christensen, Charlotte R., Cohen, Roger E., Quinn, Thomas R., Wadsley, James
We use a sample of 73 simulated satellite and central dwarf galaxies spanning a stellar mass range of $10^{5.3}-10^{9.1} M_\odot$ to investigate the origin of their stellar age gradients. We find that dwarf galaxies often form their stars "inside-out
Externí odkaz:
http://arxiv.org/abs/2408.10379
Autor:
Azartash-Namin, Bianca, Engelhardt, Anna, Munshi, Ferah, Keller, B. W., Brooks, Alyson M., Van Nest, Jordan, Christensen, Charlotte R., Quinn, Tom, Wadsley, James
We use high-resolution cosmological simulations to compare the effect of bursty star formation histories on dwarf galaxy structure for two different subgrid supernovae (SNe) feedback models in dwarf galaxies with stellar masses from $5000 <$ M$_*$/M$
Externí odkaz:
http://arxiv.org/abs/2401.06041
Autor:
Christensen, Charlotte R., Brooks, Alyson, Munshi, Ferah, Riggs, Claire, Van Nest, Jordan, Akins, Hollis, Quinn, Thomas R, Chamberland, Lucas
We are entering an era in which we will be able to detect and characterize hundreds of dwarf galaxies within the Local Volume. It is already known that a strong dichotomy exists in the gas content and star formation properties of field dwarf galaxies
Externí odkaz:
http://arxiv.org/abs/2311.04975
Autor:
Sanchez, N. Nicole, Werk, Jessica K., Christensen, Charlotte, Telford, O. Grace, Tremmel, Michael, Quinn, Thomas, Mead, Jennifer, Sharma, Ray, Brooks, Alyson
The interaction between supermassive black hole (SMBH) feedback and the circumgalactic medium (CGM) continues to be an open question in galaxy evolution. In our study, we use SPH simulations to explore the impact of SMBH feedback on galactic metal re
Externí odkaz:
http://arxiv.org/abs/2305.07672
Autor:
Van Nest, Jordan, Munshi, Ferah, Christensen, Charlotte, Brooks, Alyson M., Tremmel, Michael, Quinn, Thomas R.
We study satellite counts and quenched fractions for satellites of Milky Way analogs in Romulus25, a large-volume cosmological hydrodynamic simulation. Depending on the definition of a Milky Way analog, we have between 66 and 97 Milky Way analogs in
Externí odkaz:
http://arxiv.org/abs/2304.02007
Autor:
Kalogeropoulos, Konstantinos, Rosca, Vlad, O'Brien, Carol, Christensen, Charlotte Risager, Grahadi, Rahmat, Sørensen, Christoffer Vinther, Overath, Max D., Espi, Diego Ruiz, Jenkins, David E., Keller, Ulrich auf dem, Laustsen, Andreas H., Fryer, Thomas J., Jenkins, Timothy P.
Publikováno v:
In Toxicon 6 November 2024 250
Autor:
Bracken, Anna M., Christensen, Charlotte, O'Riain, M. Justin, Fürtbauer, Ines, King, Andrew J.
Publikováno v:
In Animal Behaviour September 2024 215:97-109
Autor:
Johnson, James W., Weinberg, David H., Vincenzo, Fiorenzo, Bird, Jonathan C., Loebman, Sarah R., Brooks, Alyson M., Quinn, Thomas R., Christensen, Charlotte R., Griffith, Emily J.
We develop a hybrid model of galactic chemical evolution that combines a multi-ring computation of chemical enrichment with a prescription for stellar migration and the vertical distribution of stellar populations informed by a cosmological hydrodyna
Externí odkaz:
http://arxiv.org/abs/2103.09838
Autor:
Bellovary, Jillian M., Hayoune, Sarra, Chafla, Katheryn, Vincent, Donovan, Brooks, Alyson, Christensen, Charlotte, Munshi, Ferah, Tremmel, Michael, Quinn, Thomas R., Van Nest, Jordan, Sligh, Serena K., Luzuriaga, Michelle
Massive black holes often exist within dwarf galaxies, and both simulations and observations have shown that a substantial fraction of these may be off-center with respect to their hosts. We trace the evolution of off-center massive black holes (MBHs
Externí odkaz:
http://arxiv.org/abs/2102.09566
Autor:
Munshi, Ferah, Brooks, Alyson, Applebaum, Elaad, Christensen, Charlotte, Sligh, Jordan P., Quinn, T.
We predict the stellar mass -- halo mass (SMHM) relationship for dwarf galaxies, using simulated galaxies with peak halo masses of M$_{\rm peak} = 10^{11}$ M$_{\odot}$ down into the ultra-faint dwarf range to M$_{\rm peak} =$ 10$^7$ M$_{\odot}$. Our
Externí odkaz:
http://arxiv.org/abs/2101.05822