Models of galaxy collisions in Stephan`s Quintet and other
... very simplified by modern standards (considering only the inverse-square force of gravity and ignoring anything else, for example self-gravity), however, they convincingly illustrated the formation of narrow elongated tidal features (so called tidal “bridges” and “tails”) from the model disks (see F ...
... very simplified by modern standards (considering only the inverse-square force of gravity and ignoring anything else, for example self-gravity), however, they convincingly illustrated the formation of narrow elongated tidal features (so called tidal “bridges” and “tails”) from the model disks (see F ...
Multiple minor mergers: formation of elliptical galaxies and
... nearly at the same time, and have comparable masses, so that the merger of only two of them would already have resulted in the formation of an elliptical galaxy. In this paper, we study a different process: the multiple, sequential mergers of the intermediate and minor types – hereafter both called ...
... nearly at the same time, and have comparable masses, so that the merger of only two of them would already have resulted in the formation of an elliptical galaxy. In this paper, we study a different process: the multiple, sequential mergers of the intermediate and minor types – hereafter both called ...
The Colors of the Universe - Naples Free-Net
... shine due to radiation from these hot, young stars; however the actual number of stars in the nebula is much higher -up to 800. It's also one of the youngest clusters known, with an age of just 1 million years. 22. M51 ...
... shine due to radiation from these hot, young stars; however the actual number of stars in the nebula is much higher -up to 800. It's also one of the youngest clusters known, with an age of just 1 million years. 22. M51 ...
... that happen to have a prominent disk around them [and] ellipticals as bulges that for some reason have missed the opportunity to acquire or maintain a prominent disk.” We adopt this point of view. However, as observations improve, we discover more and more features that make it difficult to interpre ...
Isolated elliptical galaxies in the local Universe
... fraction of ellipticals with younger stellar populations is predicted than in clusters (Kauffmann 1996; Niemi et al. 2010). This may indicate different formation histories. Theoretical models suggest that ellipticals in clusters form through dissipative infall of gas and numerous mergers that took pla ...
... fraction of ellipticals with younger stellar populations is predicted than in clusters (Kauffmann 1996; Niemi et al. 2010). This may indicate different formation histories. Theoretical models suggest that ellipticals in clusters form through dissipative infall of gas and numerous mergers that took pla ...
The redshift evolution of the distribution of star formation among dark
... values are given in B12. We checked that our results are not modified significantly if we use the double-Schechter fits of the measured SMF of Ilbert et al. (2013) instead of this simplified parametric form. To correctly populate dark matter halos, we also need to account for the population of non-s ...
... values are given in B12. We checked that our results are not modified significantly if we use the double-Schechter fits of the measured SMF of Ilbert et al. (2013) instead of this simplified parametric form. To correctly populate dark matter halos, we also need to account for the population of non-s ...
THE UV-OPTICAL COLOR MAGNITUDE DIAGRAM. II. PHYSICAL
... redshift confidence zconf > 0:67. The sample was limited to regions of sky with UV exposure times greater than 800 s, location on-detector within 0.55 of field center, an NUV magnitude cut (16 < NUV < 23) and non-artifacts using nuv_artifact 1. These cuts, source matching, and completeness are al ...
... redshift confidence zconf > 0:67. The sample was limited to regions of sky with UV exposure times greater than 800 s, location on-detector within 0.55 of field center, an NUV magnitude cut (16 < NUV < 23) and non-artifacts using nuv_artifact 1. These cuts, source matching, and completeness are al ...
Document
... – Bias factor of quasars average DM halo mass – Clustering probably provides the most effective probe to the statistical properties of quasar host galaxies at high-redshift – Combining with quasar density quasar lifetime and duty cycle ...
... – Bias factor of quasars average DM halo mass – Clustering probably provides the most effective probe to the statistical properties of quasar host galaxies at high-redshift – Combining with quasar density quasar lifetime and duty cycle ...
lecture
... Two types of outer rings: (depending on initial gas distribution) - parallel to the bar uniform gas distribution extending well beyond OLR - perpendicular to the bar more concentrated distribution (Most observed outer rings are perpendicular to the bar, e.g., Kormendy, ...
... Two types of outer rings: (depending on initial gas distribution) - parallel to the bar uniform gas distribution extending well beyond OLR - perpendicular to the bar more concentrated distribution (Most observed outer rings are perpendicular to the bar, e.g., Kormendy, ...
Galaxy pairs in the Sloan Digital Sky Survey III. Evidence of induced
... et al. 2010), even if the interactions do not lead to mergers. Several lines of observational evidence indicate that interaction-induced star formation tends to be centrally concentrated. Bergvall, Laurikainen & Aalto (2003) and Park & Choi (2009) use optical colours to infer that star formation is ...
... et al. 2010), even if the interactions do not lead to mergers. Several lines of observational evidence indicate that interaction-induced star formation tends to be centrally concentrated. Bergvall, Laurikainen & Aalto (2003) and Park & Choi (2009) use optical colours to infer that star formation is ...
Probing nuclear activity versus star formation at z ∼ 0.8 using near
... or obscured optical-to-infrared (IR) SEDs instead, practically indistinguishable from those of spiral/starburst galaxies (Alonso-Herrero et al. 2004, 2008; Rigby et al. 2006; Trump et al. 2009). The star formation activity in the hosts of AGN at z ∼ 1 has been studied by several authors using mid-in ...
... or obscured optical-to-infrared (IR) SEDs instead, practically indistinguishable from those of spiral/starburst galaxies (Alonso-Herrero et al. 2004, 2008; Rigby et al. 2006; Trump et al. 2009). The star formation activity in the hosts of AGN at z ∼ 1 has been studied by several authors using mid-in ...
Identifying the progenitor set of present-day early
... We present a comprehensive theoretical study, using a semi-analytical model within the standard LCDM framework, of the photometric properties of the progenitors of present-day early-type galaxies in the redshift range 0 < z < 1. We explore progenitors of all morphologies and study their characterist ...
... We present a comprehensive theoretical study, using a semi-analytical model within the standard LCDM framework, of the photometric properties of the progenitors of present-day early-type galaxies in the redshift range 0 < z < 1. We explore progenitors of all morphologies and study their characterist ...
Stars and Galaxies PowerPoint
... hundreds to thousands of galaxies, 60 million lightyears away giant elliptical at center, formed by galactic cannibalism the Local Group is “falling” toward the Virgo Cluster at 60 to 250 miles per second! ...
... hundreds to thousands of galaxies, 60 million lightyears away giant elliptical at center, formed by galactic cannibalism the Local Group is “falling” toward the Virgo Cluster at 60 to 250 miles per second! ...
Stars and Galaxies - Lunar and Planetary Institute
... hundreds to thousands of galaxies, 60 million lightyears away giant elliptical at center, formed by galactic cannibalism the Local Group is “falling” toward the Virgo Cluster at 60 to 250 miles per second! ...
... hundreds to thousands of galaxies, 60 million lightyears away giant elliptical at center, formed by galactic cannibalism the Local Group is “falling” toward the Virgo Cluster at 60 to 250 miles per second! ...
ROSAT Ian R. Stevens* and David K. Strickland*
... superimposed on the Digitized Sky Survey image. The X-ray contours are from the longer 6.2-ks observation only. As noted by Turner et al. (1993), there are several point sources in the vicinity of the nucleus of NGC 1365. In addition to a strong central point source there is also low-surface-brightn ...
... superimposed on the Digitized Sky Survey image. The X-ray contours are from the longer 6.2-ks observation only. As noted by Turner et al. (1993), there are several point sources in the vicinity of the nucleus of NGC 1365. In addition to a strong central point source there is also low-surface-brightn ...
Preliminary Talk Abstract Book - MoCA
... studies of the build-up of the red sequence and of the morphological transformation of galaxies in a sample of 9 clusters at 0.8 < z < 1.5 from the HAWK-I Cluster Survey (HCS). The comparison with the z 0.05 clusters of the WINGS survey shows that the cluster red sequence was already assembled at z ...
... studies of the build-up of the red sequence and of the morphological transformation of galaxies in a sample of 9 clusters at 0.8 < z < 1.5 from the HAWK-I Cluster Survey (HCS). The comparison with the z 0.05 clusters of the WINGS survey shows that the cluster red sequence was already assembled at z ...
Common BH/SFR Evolution
... Obscured Accretion • Critical stage of BH-galaxy connection. • Occurs when galaxies form most of their stars. • Can represent up to 50% of matter accretion onto the central black hole. ...
... Obscured Accretion • Critical stage of BH-galaxy connection. • Occurs when galaxies form most of their stars. • Can represent up to 50% of matter accretion onto the central black hole. ...
The correlation between galaxy morphology and star
... universe. Several surveys that have used the Hubble Space Telescope (HST) have observed that the properties of galaxies at z ∼ 1 are broadly consistent with those in the local universe (Bell et al. 2004: GEMS, Papovich et al. 2005: HDFN, Cassata et al. 2007 : COSMOS). However, the morphological anal ...
... universe. Several surveys that have used the Hubble Space Telescope (HST) have observed that the properties of galaxies at z ∼ 1 are broadly consistent with those in the local universe (Bell et al. 2004: GEMS, Papovich et al. 2005: HDFN, Cassata et al. 2007 : COSMOS). However, the morphological anal ...
Galaxy Morphology - The University of Alabama
... early galaxy classification was based on photographic plates taken in the blue region of the spectrum. Silver bromide dry emulsion plates were the staple of astronomy beginning in the 1870s and were relatively more sensitive to blue light than to red light. Later, photographs taken with Kodak 103a-O ...
... early galaxy classification was based on photographic plates taken in the blue region of the spectrum. Silver bromide dry emulsion plates were the staple of astronomy beginning in the 1870s and were relatively more sensitive to blue light than to red light. Later, photographs taken with Kodak 103a-O ...
Star Formation in Galaxies Along the Hubble Sequence
... given object dictated by the ratio of early to late-type stars, or alternatively by the ratio of young (< 1 Gyr) to old (3–15 Gyr) stars. This makes it possible to use the observed colors to estimate the fraction of young stars and the mean SFR over the past 108 –109 years. The simplest application ...
... given object dictated by the ratio of early to late-type stars, or alternatively by the ratio of young (< 1 Gyr) to old (3–15 Gyr) stars. This makes it possible to use the observed colors to estimate the fraction of young stars and the mean SFR over the past 108 –109 years. The simplest application ...
Proper Motion of the Andromeda Galaxy
... All masers seen in the Galaxy occur in other galaxies. But, moving from kpc to Mpc distances, Resolution down 1000-fold Sensitivity down 106-fold 1 pc → 1 kpc 1 Jy → 1 µJy Only a few species (water best) Only a few 10’s of galaxies ...
... All masers seen in the Galaxy occur in other galaxies. But, moving from kpc to Mpc distances, Resolution down 1000-fold Sensitivity down 106-fold 1 pc → 1 kpc 1 Jy → 1 µJy Only a few species (water best) Only a few 10’s of galaxies ...
THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES
... type over the largely unexplored redshift range 0.1 < ∼z< ∼ 0.5. Because only the closest or brightest of the galaxies are individually detected in X-rays, we use a stacking analysis to determine the mean properties of the sample. Our results suggest that X-ray emission from spectroscopically late-t ...
... type over the largely unexplored redshift range 0.1 < ∼z< ∼ 0.5. Because only the closest or brightest of the galaxies are individually detected in X-rays, we use a stacking analysis to determine the mean properties of the sample. Our results suggest that X-ray emission from spectroscopically late-t ...
2. The X-ray-Radio correlation for bulgeless galaxies
... Correlations between the X-ray and Radio emissions are observed for both galaxies with Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass o ...
... Correlations between the X-ray and Radio emissions are observed for both galaxies with Active Galactic Nuclei (AGN) and in Star Forming galaxies. For the first case, the Xray/Radio correlation seems to present different slopes for Radio-loud and Radio-quiet AGN and may be used to estimate the mass o ...
Observational evidence for AGN feedback in early
... Key in our approach is the use of a purely morphological selection criterion through visual inspection which produces a sample that is not biased against recent star formation and nuclear activity. Based on the nebular emission-line characteristics we separate between star formation activity, black ...
... Key in our approach is the use of a purely morphological selection criterion through visual inspection which produces a sample that is not biased against recent star formation and nuclear activity. Based on the nebular emission-line characteristics we separate between star formation activity, black ...
Chapter 15 ppt
... • Galaxies are composed of stars, planetary systems, nebulas, and star clusters. • Looking at distant galaxies reveals what young galaxies looked like. ...
... • Galaxies are composed of stars, planetary systems, nebulas, and star clusters. • Looking at distant galaxies reveals what young galaxies looked like. ...
Atlas of Peculiar Galaxies
The Atlas of Peculiar Galaxies is a catalog of peculiar galaxies produced by Halton Arp. A total of 338 galaxies are presented in the atlas, which was originally published in 1966 by the California Institute of Technology.The primary goal of the catalog was to present photographs of examples of the different kinds of peculiar structures found among nearby galaxies. Arp realized that the reason why galaxies formed into spiral or elliptical shapes was not well understood. He perceived peculiar galaxies as small ""experiments"" that astronomers could use to understand the physical processes that distort spiral or elliptical galaxies. With this atlas, astronomers had a sample of peculiar galaxies that they could study in more detail. The atlas does not present a complete overview of every peculiar galaxy in the sky but instead provides examples of the different phenomena as observed in nearby galaxies.Because little was known at the time of publication about the physical processes that caused the different shapes, the galaxies in the atlas are sorted based on their appearance. Objects 1–101 are individual peculiar spiral galaxies or spiral galaxies that apparently have small companions. Objects 102–145 are elliptical and elliptical-like galaxies. Individual or groups of galaxies with neither elliptical nor spiral shapes are listed as objects 146–268. Objects 269–327 are double galaxies. Finally, objects that simply do not fit into any of the above categories are listed as objects 332–338. Most objects are best known by their other designations, but a few galaxies are best known by their Arp numbers (such as Arp 220).Today, the physical processes that lead to the peculiarities seen in the Arp atlas are now well understood. A large number of the objects are interacting galaxies, including M51 (Arp 85), Arp 220, and the Antennae Galaxies (NGC 4038/NGC 4039, or Arp 244). A few of the galaxies are simply dwarf galaxies that do not have enough mass to produce enough gravity to allow the galaxies to form any cohesive structure. NGC 1569 (Arp 210) is an example of one of the dwarf galaxies in the atlas. A few other galaxies are radio galaxies. These objects contain active galactic nuclei that produce powerful jets of gas called radio jets. The atlas includes the nearby radio galaxies M87 (Arp 152) and Centaurus A (Arp 153).