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Journal articles on the topic 'Galaxies'

Author: Grafiati

Published: 4 June 2021

Last updated: 25 July 2025

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1

Guhathakurta, P., K. Ing, H. W. Rix, M. Colless, and T. Williams. "Spatially-Resolved Internal Kinematics of 〈z〉 ≈ 0.3 Field Galaxies: Evidence for Rotation." Symposium - International Astronomical Union 171 (1996): 385. http://dx.doi.org/10.1017/s0074180900233044.

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The nature of evolution in faint field galaxies remains a mystery. The Tully-Fisher relation, empirically relating the intrinsic luminosity of a spiral galaxy to its rotation speed, is an important tool for constraining the amount of luminosity evolution in distant field galaxies. Studying the luminosity-vs-linewidth relation for distant galaxies allows one to compare the luminosity of local and distant galaxies. The customary measure of a galaxy's rotation speed is the width of an emission line. It is important, however, to test whether the linewidth is a reliable measure of the galaxy's rota

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Bellovary, Jillian M., Sarra Hayoune, Katheryn Chafla, et al. "The origins of off-centre massive black holes in dwarf galaxies." Monthly Notices of the Royal Astronomical Society 505, no. 4 (2021): 5129–41. http://dx.doi.org/10.1093/mnras/stab1665.

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ABSTRACT Massive black holes often exist within dwarf galaxies, and both simulations and observations have shown that a substantial fraction of these may be off-centre with respect to their hosts. We trace the evolution of off-centre massive black holes (MBHs) in dwarf galaxies using cosmological hydrodynamical simulations, and show that the reason for off-centre locations is mainly due to galaxy–galaxy mergers. We calculate dynamical time-scales and show that off-centre MBHs are unlikely to sink to their galaxys’ centres within a Hubble time, due to the shape of the hosts’ potential wells and

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Miller, Tim B., and Pieter van Dokkum. "Bayesian Fitting of Multi-Gaussian Expansion Models to Galaxy Images." Astrophysical Journal 923, no. 1 (2021): 124. http://dx.doi.org/10.3847/1538-4357/ac2b30.

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Abstract Fitting parameterized models to images of galaxies has become the standard for measuring galaxy morphology. This forward-modeling technique allows one to account for the point-spread function to effectively study semi-resolved galaxies. However, using a specific parameterization for a galaxy’s surface brightness profile can bias measurements if it is not an accurate representation. Furthermore, it can be difficult to assess systematic errors in parameterized profiles. To overcome these issues we employ the Multi-Gaussian expansion (MGE) method of representing a galaxy’s profile togeth

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van Dokkum, Pieter, Zili Shen, Michael A. Keim, et al. "A trail of dark-matter-free galaxies from a bullet-dwarf collision." Nature 605, no. 7910 (2022): 435–39. http://dx.doi.org/10.1038/s41586-022-04665-6.

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AbstractThe ultra-diffuse galaxies DF2 and DF4 in the NGC 1052 group share several unusual properties: they both have large sizes1, rich populations of overluminous and large globular clusters2–6, and very low velocity dispersions that indicate little or no dark matter7–10. It has been suggested that these galaxies were formed in the aftermath of high-velocity collisions of gas-rich galaxies11–13, events that resemble the collision that created the bullet cluster14 but on much smaller scales. The gas separates from the dark matter in the collision and subsequent star formation leads to the for

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Graham, Alister W. "Resequencing the Hubble sequence and the quadratic (black hole mass)–(spheroid stellar mass) relation for elliptical galaxies." Monthly Notices of the Royal Astronomical Society 522, no. 3 (2023): 3588–601. http://dx.doi.org/10.1093/mnras/stad1124.

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ABSTRACT One of the most protracted problems in astronomy has been understanding the evolution of galaxy morphology. Much discussion has surrounded how lenticular galaxies may form a bridging population between elliptical and spiral galaxies. However, with recourse to a galaxy’s central black hole mass, accretion-built spiral galaxies have emerged as the bridging population between low-mass lenticular galaxies and the dusty merger-built lenticular galaxies contiguous with elliptical galaxies and ‘brightest cluster galaxies’ in the black hole/galaxy mass diagram. Spiral galaxies, including the

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Ludwig, Eric, Julia Falcone, Mariarosa Marinelli, William Ostling, and Charles T. Liu. "The Relation between Gas-phase Metallicity and Stellar Mass Surface Density in Post-starburst E+A and E+A+ Galaxies within the Coma Cluster Observed by the SDSS-IV MaNGA Survey." Research Notes of the AAS 6, no. 12 (2022): 259. http://dx.doi.org/10.3847/2515-5172/aca908.

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Abstract We present an analysis of the Mass–Metallicity Relation (MZR) in 29 post-starburst galaxies in the Coma Cluster. Outward from the central dominant galaxy, NGC 4889, we conducted a conical survey of all galaxies observed by the Sloan Digital Sky Survey Data Release 17 (SDSS DR17) Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey within a 5° radius and redshift constraints 0.013 < z < 0.033. We identified 21 E+A galaxies and 8 “E+A+ galaxies” whose spectra matched the criteria of an E+A galaxy, but contain Balmer emission lines, indicating star formation. We utili

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Douglass, Kelly A., and Regina Demina. "Dependence of the Ratio of Total to Visible Mass on Observable Properties of Sloan Digital Sky Survey MaNGA Galaxies." Astrophysical Journal 925, no. 2 (2022): 127. http://dx.doi.org/10.3847/1538-4357/ac3b56.

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Abstract Using spectroscopic observations from the Sloan Digital Sky Survey Mapping Nearby Galaxies at Apache Point Observatory Data Release 15, we study the relationships between the ratio of total to visible mass and various parameters characterizing the evolution and environment of the galaxies in this survey. Measuring the rotation curve with the relative velocities of the Hα emission line across a galaxy’s surface, we estimate each galaxy’s total mass. We develop a statistical model to describe the observed distribution in the ratio of total to visible mass, from which we extract the most

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Camps-Fariña, Artemi, Patricia Sánchez-Blázquez, Santi Roca-Fàbrega, and Sebastián F. Sánchez. "Variable metallicity yields as tracers of inflows." Proceedings of the International Astronomical Union 17, S373 (2021): 246–48. http://dx.doi.org/10.1017/s1743921322003982.

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AbstractPristine gas accretion is expected to be the main driver of sustained star formation in galaxies. We measure the required amount of accreted gas at each moment over a galaxy’s history to produce the observed metallicity at that time given its star-forming history. More massive galaxies tend to have higher accretion rates and a larger drop of the accretion rate towards the present time. Within the same mass bin galaxies that are currently star-forming or in the Green Valley have similar, sustained, accretion histories while retired galaxies had a steep decline in the past. Plotting the

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Jeon, Seyoung, Sukyoung K. Yi, Yohan Dubois, et al. "Star Formation History and Transition Epoch of Cluster Galaxies Based on the Horizon-AGN Simulation." Astrophysical Journal 941, no. 1 (2022): 5. http://dx.doi.org/10.3847/1538-4357/ac9d8c.

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Abstract Cluster galaxies exhibit substantially lower star formation rates than field galaxies today, but it is conceivable that clusters were sites of more active star formation in the early universe. Herein, we present an interpretation of the star formation history (SFH) of group/cluster galaxies based on the large-scale cosmological hydrodynamic simulation, Horizon-AGN. We find that massive galaxies in general have small values of e-folding timescales of star formation decay (i.e., “mass quenching”) regardless of their environment, while low-mass galaxies exhibit prominent environmental de

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Magrini, Laura, Mario Perinotto, Romano L. M. Corradi, and Antonio Mampaso. "A Search for Planetary Nebulae in M 33 and M 81." Symposium - International Astronomical Union 209 (2003): 559–60. http://dx.doi.org/10.1017/s0074180900209698.

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We present a study of the PNe systems of two nearby galaxies: the spirals M 33 and M 81. The luminosity functions (PNLFs) for the two PNe systems were built and the distances to both galaxies were given (0.84 ± 0.09 Mpc to M 33 and 3.84 ± 0.41 Mpc to M 81). The behavior of PNe excitation was examined across both galaxies, finding no evidence for substantial differences in excitation between bulge and disk PNe, nor for variations along the galaxian disks.

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Smith, Eric P., and Paul Hintzen. "Multi-Color Imaging of Selected Southern Interacting Galaxies." International Astronomical Union Colloquium 124 (1990): 55–58. http://dx.doi.org/10.1017/s0252921100004887.

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We present preliminary results from a study of selected Arp-Madore Southern Hemisphere peculiar galaxies. Broadband CCD images (BVRI) of a subset of these galaxies allow us to study each galaxy’s optical morphology, color, and (in a crude manner) degree of nuclear activity, and to compare them with similar data we possess on other active galaxies. Many of these galaxies have optical morphologies closely resembling those of powerful radio galaxies (Smith and Heckman 1989), yet their radio emission is unremarkable. Accurate positions for subsequent spectroscopic studies have been determined alon

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Correa, Camila A., Joop Schaye, and James W. Trayford. "The origin of the red-sequence galaxy population in the EAGLE simulation." Monthly Notices of the Royal Astronomical Society 484, no. 4 (2019): 4401–12. http://dx.doi.org/10.1093/mnras/stz295.

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ABSTRACT We investigate the evolution in colour and morphology of the progenitors of red-sequence galaxies in the EAGLE cosmological hydrodynamical simulation. We quantify colours with u* − r* intrinsic magnitudes and morphologies with a measure of the stellar kinematics. The time when galaxies moved on to the red sequence depends on their morphology. Disc-type galaxies tend to have become red during the last 3 Gyr, while elliptical-type galaxies joined the red sequence earlier, with half the sample already being red 5 Gyr ago. The time-scale, τGreen, of colour transition through the ‘green va

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Artale, M. Celeste, Michela Mapelli, Yann Bouffanais, Nicola Giacobbo, Mario Pasquato, and Mario Spera. "Mass and star formation rate of the host galaxies of compact binary mergers across cosmic time." Monthly Notices of the Royal Astronomical Society 491, no. 3 (2019): 3419–34. http://dx.doi.org/10.1093/mnras/stz3190.

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ABSTRACT We investigate the properties of the host galaxies of compact binary mergers across cosmic time, by means of population-synthesis simulations combined with galaxy catalogues from the eagle suite. We analyse the merger rate per galaxy of binary neutron stars (BNSs), black hole–neutron star binaries (BHNSs), and binary black holes (BBHs) from redshift zero up to six. The binary merger rate per galaxy strongly correlates with the stellar mass of the host galaxy at any redshift considered here. This correlation is significantly steeper for BNSs than for both BHNSs and BBHs. Moreover, we f

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Feng, Shuai, Shi-Yin Shen, Fang-Ting Yuan, Y. Sophia Dai, and Karen L. Masters. "The Velocity Map Asymmetry of Ionized Gas in MaNGA. I. The Catalog and General Properties." Astrophysical Journal Supplement Series 262, no. 1 (2022): 6. http://dx.doi.org/10.3847/1538-4365/ac80f2.

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Abstract The SDSS-IV MaNGA survey has measured two-dimensional maps of emission-line velocities for a statistically powerful sample of nearby galaxies. The asymmetric features of these kinematics maps reflect the nonrotational component of a galaxy’s internal motion of ionized gas. In this study, we present a catalog of kinematic asymmetry measurements of the Hα velocity map of a sample of 5353 MaNGA galaxies. Based on this catalog, we find that “special” galaxies (e.g., merging galaxies, barred galaxies, and active galactic nucleus host galaxies) contain more galaxies with highly asymmetric v

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Comerford, Julia M., James Negus, R. Scott Barrows, et al. "Toward a More Complete Optical Census of Active Galactic Nuclei via Spatially Resolved Spectroscopy." Astrophysical Journal 927, no. 1 (2022): 23. http://dx.doi.org/10.3847/1538-4357/ac496a.

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Abstract While emission line flux ratio diagnostics are the most common technique for identifying active galactic nuclei (AGNs) in optical spectra, applying this approach to single-fiber spectra of galaxies can omit entire subpopulations of AGNs. Here, we use spatially resolved spectroscopy from the Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey to construct a sample of 10 galaxies where Baldwin–Philips–Terlevich line flux ratio diagnostics classify each galaxy’s central 3″ spectrum as LINER or star-forming, while >10% of the spaxels in the galaxy’s MaNGA footprint are c

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Drory, Niv, and David B. Fisher. "A connection between bulge properties and the bimodality of galaxies." Proceedings of the International Astronomical Union 3, S245 (2007): 67–70. http://dx.doi.org/10.1017/s1743921308017304.

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AbstractThe global colors and structure of galaxies have recently been shown to follow bimodal distributions. Galaxies separate into a “red sequence”, populated prototypically by early-type galaxies, and a “blue cloud”, whose typical objects are late-type disk galaxies. Intermediate-type (Sa-Sbc) galaxies populate both regions. It has been suggested that this bimodality reflects the two-component nature of disk-bulge galaxies. However, it has now been established that there are two types of bulges: “classical bulges” that are dynamically hot systems resembling (little) ellipticals, and “pseudo

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Sofue, Yoshiaki, and Asao Habe. "Formation of Galactic Bulges by Starbursts and the Origin of Hubble Morphological Types." Publications of the Astronomical Society of Japan 44, no. 3 (1992): 325–29. https://doi.org/10.1093/pasj/44.3.325.

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Abstract We point out a possibility that a significant fraction of galactic bulge stars are formed from gas clouds ejected by starbursts in the central regions of galaxies. Stronger bursts result in larger and more extended bulges, and therefore lead to early type galaxies, and vice versa. The Hubble morphological types can be understood in terms of primeval starburst history of individual galaxies. Since the burst strength depends on the strength of tidal interaction, Hubble types inevitably depend on the galaxian number density, which explains the density-morphology relation.

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Courteau, Stéphane, and Aaron A. Dutton. "The Mass Distribution in Disk Galaxies." Proceedings of the International Astronomical Union 11, A29B (2015): 195–96. http://dx.doi.org/10.1017/s1743921316004865.

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AbstractWe present the relative fraction of baryons and dark matter at various radii in galaxies. For spiral galaxies, this fraction measured in a galaxy's inner parts is typically baryon-dominated (maximal) and dark-matter dominated (sub-maximal) in the outskirts. The transition from maximal to sub-maximal baryons occurs within the inner parts of low-mass disk galaxies (with Vtot ≤ 200 km s−1) and in the outer disk for more massive systems. The mean mass fractions for late- and early-type galaxies vary significantly at the same fiducial radius and circular velocity, suggesting a range of gala

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Peterken, Thomas, Alfonso Aragón-Salamanca, Michael Merrifield, et al. "Size, shade, or shape? The contribution of galaxies of different types to the star formation history of the Universe from SDSS-IV MaNGA." Monthly Notices of the Royal Astronomical Society 502, no. 3 (2021): 3128–43. http://dx.doi.org/10.1093/mnras/stab268.

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ABSTRACT By fitting stellar populations to the fourth generation of the Sloan Digital Sky Survey (SDSS-IV) Mapping Nearby Galaxies at Apache Point Observatory (MaNGA) survey observations of ∼7000 suitably weighted individual galaxies, we reconstruct the star formation history of the Universe, which we find to be in reasonable agreement with previous studies. Dividing the galaxies by their present-day stellar mass, we demonstrate the downsizing phenomenon, whereby the more massive galaxies hosted the most star formation at earlier times. Further dividing the galaxy sample by colour and morpholo

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Adams, Dominic, Hugh Dickinson, Lucy Fortson, et al. "The Prevalence of Star-forming Clumps as a Function of Environmental Overdensity in Local Galaxies." Astrophysical Journal 979, no. 2 (2025): 118. https://doi.org/10.3847/1538-4357/ad7119.

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Abstract 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. By comparison, ≲5% of local star-forming galaxies host comparable clumps. In this work, we investigate the link between the environmental conditions surrounding local (z < 0.04) galaxies and the prevalence of clumps in these galaxies. To obtain our clump sample, we use a Faster R-CNN object detection network trained on the catalog of clump labels provided by the Galaxy Zoo: Clump Scout proj

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Bertola, F., S. Okamura, C. Balkowski, et al. "Commission 28: Galaxies: (Galaxies)." Transactions of the International Astronomical Union 24, no. 1 (2000): 299–310. http://dx.doi.org/10.1017/s0251107x00003230.

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This report covers the period July 1996 to June 1999. It has been prepared by the President of the Commission with contributions from the members of the Organizing Committee and Dr. E.M. Corsini. As discussed in Kyoto and decided by the Organizing Committee, the report is meant to be in the “short” version.

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Okamura, Sadanori. "Commission 28: Galaxies (Galaxies)." Transactions of the International Astronomical Union 25, no. 2 (2007): 171–72. http://dx.doi.org/10.1017/s0251107x00026766.

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Okamura, S., E. Sadler, C. Balkowski, et al. "Commission 28: Galaxies: (Galaxies)." Transactions of the International Astronomical Union 25, no. 1 (2002): 313–16. http://dx.doi.org/10.1017/s0251107x00001620.

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Hamabata, Akinari, Taira Oogi, Masamune Oguri, Takahiro Nishimichi, and Masahiro Nagashima. "New constraints on red-spiral galaxies from their kinematics in clusters of galaxies." Monthly Notices of the Royal Astronomical Society 488, no. 3 (2019): 4117–25. http://dx.doi.org/10.1093/mnras/stz1991.

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ABSTRACTThe distributions of the pairwise line-of-sight velocity between galaxies and their host clusters are segregated according to the galaxy’s colour and morphology. We investigate the velocity distribution of red-spiral galaxies, which represents a rare population within galaxy clusters. We find that the probability distribution function of the pairwise line-of-sight velocity vlos between red-spiral galaxies and galaxy clusters has a dip at vlos = 0, which is a very odd feature, at 93 per cent confidence level. To understand its origin, we construct a model of the phase-space distribution

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Siegel, Jared C., and Peter Melchior. "Spatially Resolved Galaxy–Dust Modeling with Coupled Data-driven Priors." Astrophysical Journal 986, no. 2 (2025): 212. https://doi.org/10.3847/1538-4357/add3f9.

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Abstract A notorious problem in astronomy is the recovery of the true shape and spectral energy distribution (SED) of a galaxy despite attenuation by interstellar dust embedded in the same galaxy. This problem has been solved for a few hundred nearby galaxies with exquisite data coverage, but these techniques are not scalable to the billions of galaxies soon to be observed by large wide-field surveys like the Legacy Survey of Space and Time, Euclid, and Roman. We present a method for jointly modeling the spatially resolved stellar and dust properties of galaxies from multiband images. To captu

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Kovlakas, K., A. Zezas, J. J. Andrews, et al. "A census of ultraluminous X-ray sources in the local Universe." Monthly Notices of the Royal Astronomical Society 498, no. 4 (2020): 4790–810. http://dx.doi.org/10.1093/mnras/staa2481.

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ABSTRACT Using the Chandra Source Catalog 2.0 and a newly compiled catalogue of galaxies in the local Universe, we deliver a census of ultraluminous X-ray source (ULX) populations in nearby galaxies. We find 629 ULX candidates in 309 galaxies with distance smaller than 40 Mpc. The foreground/background contamination is $\sim \! 20{{\ \rm per\ cent}}$. The ULX populations in bona fide star-forming galaxies scale on average with star formation rate and stellar mass (M⋆) such that the number of ULXs per galaxy is $0.45^{+0.06}_{-0.09}\times \frac{\rm SFR}{\rm M_\odot \, yr^{-1}}{+}3.3^{+3.8}_{-3.

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Fraser-McKelvie, Amelia, Alfonso Aragón-Salamanca, Michael Merrifield, et al. "SDSS-IV MaNGA: spatially resolved star formation in barred galaxies." Monthly Notices of the Royal Astronomical Society 495, no. 4 (2020): 4158–69. http://dx.doi.org/10.1093/mnras/staa1416.

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ABSTRACT Bars inhabit the majority of local-Universe disc galaxies and may be important drivers of galaxy evolution through the redistribution of gas and angular momentum within discs. We investigate the star formation and gas properties of bars in galaxies spanning a wide range of masses, environments, and star formation rates using the Mapping Nearby Galaxies at APO galaxy survey. Using a robustly defined sample of 684 barred galaxies, we find that fractional (or scaled) bar length correlates with the host’s offset from the star formation main sequence. Considering the morphology of the Hα e

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Tchernyshyov, Kirill, Jessica K. Werk, Matthew C. Wilde, et al. "The CGM² Survey: Quenching and the Transformation of the Circumgalactic Medium." Astrophysical Journal 949, no. 2 (2023): 41. http://dx.doi.org/10.3847/1538-4357/acc86a.

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Abstract This study addresses how the incidence rate of strong O vi absorbers in a galaxy’s circumgalactic medium (CGM) depends on galaxy mass and, independently, on the amount of star formation in the galaxy. We use Hubble Space Telescope/Cosmic Origins Spectrograph absorption spectroscopy of quasars to measure O vi absorption within 400 projected kpc and 300 km s−1 of 52 galaxies with M * ∼ 3 × 1010 M ⊙. The galaxies have redshifts 0.12 < z < 0.6, stellar masses 1010.1 M ⊙ < M * < 1010.9 M ⊙, and spectroscopic classifications as star-forming or passive. We compare the incidence r

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Witherspoon, Catherine A., and Eric M. Wilcots. "Environment of Quiescent Low-mass Galaxies Hosting AGNs in MaNGA." Astrophysical Journal 961, no. 2 (2024): 192. http://dx.doi.org/10.3847/1538-4357/acfca8.

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Abstract The discovery of active galactic nuclei (AGNs) in low-mass (M * ≤ 5 × 109 M ⊙) galaxies has pushed forward the idea that AGN feedback may play a role in quenching star formation in the low-mass regime. In order to test whether AGNs can be a dominant quenching mechanism, we must first disentangle the effects of internal and external processes caused by a galaxy’s environment. We have used the Sloan Digital Sky Survey IV Mapping Nearby Galaxies at Apache Point Observatory survey to produce resolved Baldwin, Phillips, & Terlevich diagrams, and we find 41 AGNs (∼1.3%) in low-mass gala

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Feldmeier-Krause, A., I. Lonoce, and W. L. Freedman. "Stellar Population and Elemental Abundance Gradients of Early-type Galaxies*." Astrophysical Journal 923, no. 1 (2021): 65. http://dx.doi.org/10.3847/1538-4357/ac281e.

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Abstract The evolution of galaxies is imprinted on their stellar populations. Several stellar population properties in massive early-type galaxies have been shown to correlate with intrinsic galaxy properties such as the galaxy’s central velocity dispersion, suggesting that stars formed in an initial collapse of gas (z ∼ 2). However, stellar populations change as a function of galaxy radius, and it is not clear how local gradients of individual galaxies are influenced by global galaxy properties and galaxy environment. In this paper, we study the stellar populations of eight early-type galaxie

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Groves, Brent, and Eva Schinnerer. "Dust as a tracer of gas in galaxies." Proceedings of the International Astronomical Union 10, S309 (2014): 318. http://dx.doi.org/10.1017/s174392131401014x.

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AbstractWe use a sample of 36 galaxies to study empirical relations between Herschel infrared (IR) luminosities and the total mass of the interstellar gas (H2 + HI). Such a comparison provides a simple empirical relationship without introducing the uncertainty of dust model fitting. We find tight correlations, and provide fits to these relations, between Herschel luminosities and the total gas mass integrated over entire galaxies, with the tightest, almost linear, correlation found for the longest wavelength data (SPIRE500). However, we find that accounting for the gas-phase metallicity (affec

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Yoifoi, Ponlawat, and Wichean Kriwattanawong. "Galaxy evolution in different environments along redshift within the local universe z < 0.8." Journal of Physics: Conference Series 2145, no. 1 (2021): 012002. http://dx.doi.org/10.1088/1742-6596/2145/1/012002.

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Abstract This study presents the evolution of the galaxies in different matter density along redshift within the local universe. A sample of 702,352 galaxies was collected from the Sloan Digital Sky Survey (SDSS). Under the limitation of the spectroscopic data, the appropriate photometric redshift was used to represent the spectroscopic redshift in the range of 0.0 ≤ z ≤ 0.8. Number density of galaxies, galaxy’s colors, and star formation activities are considered to describe the evolution of galaxies. In summary, the number density is not clearly different although the Dec and RA of the sky a

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Cramer, W. J., A. G. Noble, G. Rudnick, et al. "Resolved UV and Optical Color Gradients Reveal Environmental Influence on Galaxy Evolution at Redshift z ∼ 1.6." Astrophysical Journal 975, no. 1 (2024): 144. http://dx.doi.org/10.3847/1538-4357/ad7798.

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Abstract The changes in colors across a galaxy are intimately connected to the galaxy’s formation, growth, quenching history, and dust content. A particularly important epoch in the growth of galaxies is near z ∼ 2, often referred to as “cosmic noon,” where galaxies on average reach the peak of their star formation. We study a population of 125 cluster galaxies at z ∼ 1.6 in three Hubble Space Telescope filters, F475W, F625W, and F160W, roughly corresponding to the rest-frame far-ultraviolet, near-ultraviolet, and r band, respectively. By comparing to a control sample of 200 field galaxies at

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González Delgado, R. M., E. Pérez, R. Cid Fernandes, et al. "The growth of mass and metallicity in bulges and disks: CALIFA perspective." Proceedings of the International Astronomical Union 10, H16 (2012): 338. http://dx.doi.org/10.1017/s1743921314006024.

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AbstractCALIFA (Calar Alto Legacy Integral Field Area) is a 3D spectroscopic survey of 600 nearby galaxies that we are obtaining with PPaK@3.5m at Calar Alto (Sánchez et al. 2012; Husemann et al. 2012). This pioneer survey is providing valuable clues on how the mass and metallicity grow in the different galactic spatial sub-components (“bulge” and “disk”). Processed through spectral synthesis techniques, CALIFA datacubes allow us to, for the first time, spatially resolve the star formation history of galaxies (Cid Fernandes et al. 2012). The richness of this approach is already evident from th

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Aguerri, J. A. L., M. Girardi, I. Agulli, A. Negri, C. Dalla Vecchia, and L. Domínguez Palmero. "Deep spectroscopy in nearby galaxy clusters – V. The Perseus cluster." Monthly Notices of the Royal Astronomical Society 494, no. 2 (2020): 1681–92. http://dx.doi.org/10.1093/mnras/staa800.

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ABSTRACT Dwarfs are the largest population of galaxies in number in the nearby Universe. Deep spectroscopic data are still missing to obtain a better understanding of their formation and evolution processes. This study shows the results obtained from a spectroscopic campaign in the Perseus cluster. We have obtained 963 new galaxy spectra. We have measured the recessional velocity of the galaxies by using a cross-correlation technique. These data have been used to obtain the cluster membership, the dynamics of the galaxies, and the spectroscopic luminosity function (LF) of the cluster. The clus

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Keith, Blake, Ferah Munshi, Alyson M. Brooks, et al. "A MARVEL-ous Study of How Well Galaxy Shapes Reflect Dark Matter Halo Shapes in Cold Dark Matter Simulations." Astrophysical Journal 986, no. 2 (2025): 138. https://doi.org/10.3847/1538-4357/add40d.

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Abstract We present a 3D shape analysis of both dark matter (DM) and stellar matter (SM) in simulated dwarf galaxies to determine whether stellar shape traces DM shape. Using 80 central and satellite dwarf galaxies from three simulation suites (“Marvelous Massive Dwarfs,” “Marvelous Dwarfs,” and the “DC Justice League”) spanning stellar masses of 106–1010 M ⊙, we measure 3D shapes through the moment of inertia tensor at twice the effective radius to derive axis ratios (C/A and B/A) and triaxiality. We find that stellar shape does follow DM halo shape for our dwarf galaxies. However, the presen

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Amirkhanian, A. S., A. G. Egikian, H. Tiersch, and D. Stoll. "AGNs in Shakhbazian Compact Groups." International Astronomical Union Colloquium 184 (2002): 87–88. http://dx.doi.org/10.1017/s0252921100030505.

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The results of CCD spectroscopic observations of Shakhbazian compact groups of galaxies (SHCGs) with the 1.54-m (La Silla, Chile), 2.2-m (Calar Alto, Spain) and 2.6-m (Byurakan) telescopes are presented. According to these preliminary data, about 10% of member galaxies in SHCGs are emission-line galaxies (ELGs) including the broad-line AGNs (of classical Seyfert 1 type) and the narrow-emission-line galaxies.A research program has been developed in the University of Potsdam, Potsdam Astrophysikalisches Institut in cooperation with other observatories (particularly with Byurakan Astrophysical Ob

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Einasto, Jaan, Mihkel Joeveer, and Enn Saar. "Dark Matter: Observational Aspects." Symposium - International Astronomical Union 117 (1987): 243–61. http://dx.doi.org/10.1017/s0074180900150260.

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A review of observational work on dark matter in USSR is given. Dynamically the dark matter can be located (i) in the galactic disk and/or in dwarf galaxies, (ii) in coronas of galaxies and in clusters of galaxies, and (iii) distributed smoothly in voids. The possible amount of matter in all three forms is discussed. Physically dark matter can be baryonic or non-baryonic, in the latter case either hot, warm or cold. Available information on the nature of dark matter is indirect, coming from theories of the formation of structure in the Universe. Two constraints to the formation scenarios are d

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Delgado, Rosa González, Enrique Pérez, Roberto Cid Fernandes, et al. "CALIFA survey: The spatially resolved star formation history of massive galaxies." Proceedings of the International Astronomical Union 8, S295 (2012): 300–303. http://dx.doi.org/10.1017/s1743921313005097.

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AbstractThe Calar Alto Legacy Integral Field Area (CALIFA) project is an ongoing 3D spectroscopic survey of 600 nearby galaxies of all kinds. This pioneer survey is providing valuable clues on how galaxies form and evolve. Processed through spectral synthesis techniques, CALIFA datacubes allow us to, for the first time, spatially resolve the star formation history of galaxies spread across the color-magnitude diagram. The richness of this approach is already evident from the results obtained for the first ~ 1/6 of the sample. Here we show how the different galactic spatial sub-components (“bul

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Remus, Rhea-Silvia, and Duncan A. Forbes. "Accreted or Not Accreted? The Fraction of Accreted Mass in Galaxies from the Magneticum Simulations and Observations." Astrophysical Journal 935, no. 1 (2022): 37. http://dx.doi.org/10.3847/1538-4357/ac7b30.

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Abstract In the two-phase scenario of galaxy formation, a galaxy’s stellar mass growth is first dominated by in-situ star formation, and subsequently by accretion. We analyze the radial distribution of the accreted stellar mass in ∼500 galaxies from the (48 Mpc/h)3 box volume of the hydrodynamical cosmological simulation Magneticum, in a stellar-mass range of 1010 to 1012 M ⊙. We find that higher-mass galaxies have larger accreted fractions, as found in previous works, but predict generally higher accretion fractions for low-mass galaxies. Based on the 3D radial distribution of the accreted an

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Peterken, Thomas, Michael Merrifield, Alfonso Aragón-Salamanca, et al. "SDSS-IV MaNGA: when is morphology imprinted on galaxies?" Monthly Notices of the Royal Astronomical Society: Letters 500, no. 1 (2020): L42—L46. http://dx.doi.org/10.1093/mnrasl/slaa179.

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ABSTRACT It remains an open question as to how long ago the morphology that we see in a present-day galaxy was typically imprinted. Studies of galaxy populations at different redshifts reveal that the balance of morphologies has changed over time, but such snapshots cannot uncover the typical time-scales over which individual galaxies undergo morphological transformation, nor which are the progenitors of today’s galaxies of different types. However, these studies also show a strong link between morphology and star formation rate (SFR) over a large range in redshift, which offers an alternative

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Veilleux, S., J. Bland-Hawthorn, G. Cecil, and P. Shopbell. "9.18. Galactic winds in active galaxies." Symposium - International Astronomical Union 184 (1998): 417–18. http://dx.doi.org/10.1017/s0074180900085454.

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The effects of large-scale galactic winds in active galaxies may be far-reaching. It has been suggested that the Hubble sequence can be understood in terms of a galaxy's greater ability to sustain winds with increasing bulge-to-disk ratio. The large-scale circulation of gas associated with these galactic winds might help explain the mass-metallicity relation between galaxies and the metallicity-radius relation within galaxies. Galactic winds probably contribute non-negligibly to the cosmic X-ray background and may be involved in the quasar absorption-line phenomenon. The cosmological implicati

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Monachesi, A., E. F. Bell, D. J. Radburn-Smith, et al. "Resolving the stellar outskirts of six Milky Way-like galaxies beyond the Local Group." Proceedings of the International Astronomical Union 11, S321 (2016): 43. http://dx.doi.org/10.1017/s1743921316008991.

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AbstractModels of galaxy formation in a hierarchical universe predict substantial scatter in the halo-to-halo stellar properties, owing to stochasticity in galaxies’ merger histories. Currently, only few detailed observations of galaxy’s halos are available, mainly for the Milky Way and M31. The Galaxy Halos, Outer disks, Substructure, Thick disks and Star clusters (GHOSTS) HST survey is the largest study to date of the resolved stellar populations in the outskirts of disk galaxies and its observations offer a direct test of model predictions. Here we present the results we obtain for six high

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De Looze, Ilse, Jacopo Fritz, and Maarten Baes. "High-resolution, 3D radiative transfer modeling of M51." Proceedings of the International Astronomical Union 10, S309 (2014): 310. http://dx.doi.org/10.1017/s1743921314010060.

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AbstractWe present a new technique developed to model the radiative transfer (RT) effects in nearby face-on galaxies. The face-on perspective provides insight into the star-forming regions and clumpy structure, imposing the need for high-resolution 3D models to recover the asymmetric stellar and dust geometries observed in galaxies. RT modeling of the continuum emission of stars and its interaction with the embedding dust in a galaxy's interstellar medium enables a self-consistent study of the main dust heating mechanisms in galaxies. The main advantage of RT calculations is the non-local char

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Mintz, Abby, Jenny E. Greene, Erin Kado-Fong та ін. "A Nonparametric Morphological Analysis of Hα Emission in Bright Dwarfs Using the Merian Survey". Astrophysical Journal 974, № 2 (2024): 273. http://dx.doi.org/10.3847/1538-4357/ad6861.

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Abstract Using medium-band imaging from the newly released Merian Survey, we conduct a nonparametric morphological analysis of Hα emission maps and stellar continua for a sample of galaxies with 8 ≲ log ( M ⋆ / M ⊙ ) < 10.3 at 0.064 < z < 0.1. We present a novel method for estimating the stellar continuum emission through the Merian Survey’s N708 medium-band filter, which we use to measure Hα emission and produce Hα maps for our sample of galaxies with seven-band Merian photometry and available spectroscopy. We measure nonparametric morphological statistics for the Hα and stellar cont

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Sahu, Nandini, Alister Graham, and Benjamin Davis. "The Morphology-dependent Black Hole–Host Galaxy Correlations: A Consequence of Physical Formation Processes." Acta Astrophysica Taurica 3, no. 1 (2021): 39–43. http://dx.doi.org/10.31059/aat.vol3.iss1.pp39-43.

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For decades, astronomers have been investigating how the central supermassive black hole (BH) may govern the host galaxy’s properties and vice versa. Our work adds another step to this study. We have performed state-of-theart 2D modeling and multi-component photometric decompositions of the largest-to-date sample of galaxies with dynamically-measured black hole masses (MBH). The multi-component decomposition allows us to accurately extract the bulge (spheroid) stellar luminosity/mass and structural parameters (also for other galaxy components) and provides detailed galaxy morphologies. We inve

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Berek, Samantha C., Gwendolyn M. Eadie, Joshua S. 佳士 Speagle 沈, and Shu Yan Wang. "Should Zeros Count? Modeling the Galaxy–Globular Cluster Scaling Relation with(out) Zero-inflated Count Models." Astrophysical Journal 972, no. 1 (2024): 104. http://dx.doi.org/10.3847/1538-4357/ad6147.

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Abstract The scaling relation between the size of a galaxy’s globular cluster (GC) population (N GC) and the galaxy’s stellar mass (M *) is usually described with a continuous, linear model, but in reality it is a count relationship that should be modeled as such. For massive galaxies, a negative binomial (NB) model has been shown to describe the data well, but it is unclear how the scaling relation behaves at low galaxy masses where a substantial portion of galaxies have N GC = 0. In this work, we test the utility of Poisson and NB models for describing the low-mass end of the N GC−M * scalin

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Hunter, Deidre A. "Star Formation in Normal Irregular Galaxies." Symposium - International Astronomical Union 115 (1987): 611–12. http://dx.doi.org/10.1017/s0074180900096492.

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Normal, non-interacting irregular galaxies can be quite successful at forming stars. Therefore, spiral density waves are not necessary to a vigorous production of stars. Nevertheless, there is a large range in star-formation rates among irregular galaxies. Irregulars with common characteristics can have different overall levels of star-formation activity, so that the level of activity does not seem to be simple related to observable global properties of galaxian systems. The constant star formation rates of most normal irregulars also imply the existence of regulatory processes.

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Sattari, Zahra, Bahram Mobasher, Nima Chartab, et al. "Fraction of Clumpy Star-forming Galaxies at 0.5 ≤ z ≤ 3 in UVCANDELS: Dependence on Stellar Mass and Environment." Astrophysical Journal 951, no. 2 (2023): 147. http://dx.doi.org/10.3847/1538-4357/acd5d6.

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Abstract High-resolution imaging of galaxies in rest-frame UV has revealed the existence of giant star-forming clumps prevalent in high-redshift galaxies. Studying these substructures provides important information about their formation and evolution and informs theoretical galaxy evolution models. We present a new method to identify clumps in galaxies’ high-resolution rest-frame UV images. Using imaging data from CANDELS and UVCANDELS, we identify star-forming clumps in an HST/F160W ≤ 25 AB mag sample of 6767 galaxies at 0.5 ≤ z ≤ 3 in four fields, GOODS-N, GOODS-S, EGS, and COSMOS. We use a

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van Dokkum, Pieter. "The Formation & Evolution of Galaxies." Daedalus 143, no. 4 (2014): 114–24. http://dx.doi.org/10.1162/daed_a_00311.

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Weighing in at 1042 kilograms and measuring 1021 meters across, galaxies are perhaps the most awe-inspiring objects known to mankind. They are also the only places in an otherwise dark and unforgiving universe where stars and planets are able to form. In the past five to ten years we have made enormous progress in understanding when galaxies came into being and how they changed and evolved over the course of cosmic time. For the first time, we have a rudimentary idea of what our own Milky Way looked like in the distant past, and we can now simulate Milky Way–like galaxies inside powerful compu

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