共查询到20条相似文献，搜索用时 515 毫秒
1.
M. Obri&#; &#;. Ivezi&#; P. N. Best R. H. Lupton C. Tremonti J. Brinchmann M. A. Agüeros G. R. Knapp J. E. Gunn C. M. Rockosi D. Schlegel D. Finkbeiner M. Ga&#;e&#;a V. Smol&#;i&#; S. F. Anderson W. Voges M. Juri&#; R. J. Siverd W. Steinhardt A. S. Jagoda M. R. Blanton D. P. Schneider 《Monthly notices of the Royal Astronomical Society》2006,370(4):1677-1698
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L. Makarova I. Karachentsev L. Rizzi R. B. Tully G. Korotkova 《Monthly notices of the Royal Astronomical Society》2009,397(3):1672-1684
CCD photometry is presented for 20 dIrr galaxies situated in the nearby complexes CenA/M83, and CVnI as well as in the general field of the Local Volume. We present integrated magnitudes of the galaxies in B , V , I bands and also surface brightness profiles to a median isophote μ B ∼ 28 mag arcsec−2 . The popular Sersic parametrization of surface brightness profiles generally does a poor job of simultaneously fitting the inner cores and outer exponential surface brightness fall-offs observed in many of our targets. The observed sample is a part of a general project to image about 500 nearby ( D < 10 Mpc) dwarf galaxies in multiple bands. 相似文献
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We follow the chemical evolution of a galaxy through star formation and its feedback into the interstellar medium (ISM), starting from primordial gas and allowing for gas to inflow into the region being modelled. We attempt to reproduce observed spectral line strengths for early-type galaxies in order to constrain their star formation histories (SFH). The efficiencies and times of star formation are varied, as are the amount and duration of inflow. We evaluate the chemical enrichment and the mass of stars made with time. Single stellar population (SSP) data are then used to predict line strengths for composite stellar populations. The results are compared with observed line strengths in 10 ellipticals, including some features which help to break the problem of age–metallicity degeneracy in old stellar populations. We find that the elliptical galaxies modelled require high metallicity SSPs (> 3 Z⊙) at later times. In addition, the strong lines observed cannot be produced by an initial starburst in primordial gas, even if a large amount of inflow is allowed for during the first few × 108 yr. This is because some pre-enrichment is required for lines in the bulk of the stars to approach the observed line strengths in ellipticals. These strong lines are better modelled by a system with a delayed burst of star formation, following an early SFH which can be a burst or more steady star formation. Such a model is representative of star formation in normal ellipticals or spirals, respectively, followed by a starburst and gas inflow during a merger or strong interaction with a gas-rich galaxy. Alternatively, a single initial burst of normal stars with a Salpeter initial mass function could produce the observed strong lines if it followed some pre-enrichment process which did not form long-lived stars (e.g. population III stars). 相似文献
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Confirming a population of hot-dust dominated, star-forming, ultraluminous galaxies at high redshift
C. M. Casey S. C. Chapman R. J. Beswick A. D. Biggs A. W. Blain L. J. Hainline R. J. Ivison T. W. B. Muxlow Ian Smail 《Monthly notices of the Royal Astronomical Society》2009,399(1):121-128
We identify eight z > 1 radio sources undetected at 850 μm but robustly detected at 70 μm, confirming that they represent ultraluminous infrared galaxies (ULIRGs) with hotter dust temperatures (〈 T d 〉= 52 ± 10 K) than submillimetre galaxies (SMGs) at similar luminosities and redshifts. These galaxies share many properties with SMGs: ultraviolet spectra consistent with starbursts, high stellar masses and radio luminosities. We can attribute their radio emission to star formation since high-resolution Multi-Element Radio Linked Interferometer Network (MERLIN) radio maps show extended emission regions (with characteristic radii of 2–3 kpc), which are unlikely to be generated by active galactic nucleus (AGN) activity. These observations provide the first direct confirmation of hot, dusty ULIRGs which are missed by current submillimetre surveys. They have significant implications for future observations from the Herschel Space Observatory and Submillimetre Common-User Bolometer Array 2 (SCUBA2), which will select high-redshift luminous galaxies with less selection biases. 相似文献
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Neal Jackson Clive Tadhunter & William B. Sparks 《Monthly notices of the Royal Astronomical Society》1998,301(1):131-141
We present new Hubble Space Telescope ( HST ) continuum and spectral line images of the radio galaxy Cygnus A. The images show much complex structure in the central kpc2 . Continuum images show the central dust lane in detail, allowing detailed maps of E ( B − V ) to be constructed; the dust appears to follow a roughly Galactic extinction law. The emission-line components are resolved in the line images and investigated in detail. A clear 'opening cone' morphology is found, especially in the lines of Hα and [O i ]. Blue condensations are seen in the south-eastern emission component and surrounding the central region. These are almost certainly due to star formation, which began <1 Gyr ago as deduced from the colour of the regions. More extended blue continuum is also seen and corresponds to the blue polarized component detected by other recent spectropolarimetric observations. 相似文献
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Patrick F. Roche Christopher Packham Charles M. Telesco James T. Radomski Almudena Alonso-Herrero David K. Aitken Luis Colina Eric Perlman 《Monthly notices of the Royal Astronomical Society》2006,367(4):1689-1698
High spatial resolution spectroscopy at 8–13 μm with T-ReCS on Gemini-S has revealed striking variations in the mid-infrared emission and absorption in the nucleus of the Circinus galaxy (hereafter Circinus) on subarcsecond scales. The core of Circinus is compact and obscured by a substantial column of cool silicate dust. Weak extended emission to the east and west coincides with the coronal line region and arises from featureless dust grains which are probably heated by line emission in the coronal emission zone. The extended emission on the east side of the nucleus displays a much deeper silicate absorption than that on the west, indicating significant columns of cool material along the line of sight and corresponding to an additional extinction of AV ∼ 25 mag . Emission bands from aromatic hydrocarbons are not subject to this additional extinction, are relatively weak in the core and in the coronal line region, and are much more spatially extended than the continuum dust emission; they presumably arise in the circumnuclear star-forming regions. These data are interpreted in terms of an inclined disc-like structure around the nucleus extending over tens of parsecs and possibly related to the inner disc found from observations of water masers by Greenhill et al.. 相似文献
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The environmental dependence of the relations between stellar mass, structure, star formation and nuclear activity in galaxies 总被引：2，自引：0，他引：2
Guinevere Kauffmann Simon D. M. White Timothy M. Heckman Brice Ménard Jarle Brinchmann Stéphane Charlot Christy Tremonti Jon Brinkmann 《Monthly notices of the Royal Astronomical Society》2004,353(3):713-731
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Environmental effects on satellite galaxies: the link between concentration, size and colour profile 总被引：1，自引：0，他引：1
Simone M. Weinmann Guinevere Kauffmann Frank C. van den Bosch Anna Pasquali Daniel H. McIntosh Houjun Mo Xiaohu Yang Yicheng Guo 《Monthly notices of the Royal Astronomical Society》2009,394(3):1213-1228
Using the Sloan Digital Sky Survey Data Release 4 group catalogue of Yang et al., we investigate sizes, concentrations, colour gradients and surface brightness profiles of central and satellite galaxies. We compare central and satellite galaxies at fixed stellar mass, in order to disentangle environmental from stellar mass dependencies. Early- and late-type galaxies are defined according to concentration. We find that at fixed stellar mass, late-type satellite galaxies have smaller radii and larger concentrations than late-type central galaxies. No such differences are found for early-type galaxies. We have also constructed surface brightness and colour profiles for the central and satellite galaxies in our sample. We find that late-type satellite galaxies have a lower surface brightness and redder colours than late-type central galaxies. We show that all observed differences between satellite and central galaxies can be explained by a simple fading model, in which the star formation in the disc decreases over time-scales of 2–3 Gyr after a galaxy becomes a satellite. Processes that induce strong morphological changes (e.g. harassment) and processes that strip the galaxy of its entire interstellar medium need not to be invoked in order to explain the environmental dependencies we find. 相似文献
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Dimitri A. Gadotti 《Monthly notices of the Royal Astronomical Society》2009,393(4):1531-1552
We have performed 2D bulge/bar/disc decompositions using g , r and i -band images of a representative sample of nearly 1000 galaxies from the Sloan Digital Sky Survey. We show that the Petrosian concentration index is a better proxy for the bulge-to-total ratio than the global Sérsic index. We show that pseudo-bulges can be distinguished from classical bulges as outliers in the Kormendy relation. We provide the structural parameters and distributions of stellar masses of ellipticals, classical bulges, pseudo-bulges, discs and bars, and find that 32 per cent of the total stellar mass in massive galaxies in the local universe is contained in ellipticals, 36 per cent in discs, 25 per cent in classical bulges, 3 per cent in pseudo-bulges and 4 per cent in bars. Pseudo-bulges are currently undergoing intense star formation activity and populate the blue cloud of the colour–magnitude diagram. Most (though not all) classical bulges are quiescent and populate the red sequence of the diagram. Classical bulges follow a correlation between the bulge Sérsic index and bulge-to-total ratio, while pseudo-bulges do not. In addition, for a fixed bulge-to-total ratio, pseudo-bulges are less concentrated than classical bulges. Pseudo-bulges follow a mass–size relation similar to that followed by bars, and different from that followed by classical bulges. In the fundamental plane, pseudo-bulges occupy the same locus as discs. While these results point out different formation processes for classical and pseudo-bulges, we also find a significant overlap in their properties, indicating that the different processes might happen concomitantly. Finally, classical bulges and ellipticals follow offset mass–size relations, suggesting that high-mass bulges might not be simply high-mass ellipticals surrounded by discs. 相似文献
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Dimitri A. Gadotti Guinevere Kauffmann 《Monthly notices of the Royal Astronomical Society》2009,399(2):621-627
Using results from structural analysis of a sample of nearly 1000 local galaxies from the Sloan Digital Sky Survey, we estimate how the mass in central black holes is distributed amongst elliptical galaxies, classical bulges and pseudo-bulges, and investigate the relation between their stellar masses and central stellar velocity dispersion σ. Assuming a single relation between elliptical galaxy/bulge mass, M Bulge , and central black hole mass, M BH , we find that 55+8 −4 per cent of the mass in black holes in the local universe is in the centres of elliptical galaxies, 41+4 −2 per cent in classical bulges and 4+0.9 −0.4 per cent in pseudo-bulges. We find that ellipticals, classical bulges and pseudo-bulges follow different relations between their stellar masses and σ, and the most significant offset occurs for pseudo-bulges in barred galaxies. This structural dissimilarity leads to discrepant black hole masses if single M BH – M Bulge and M BH –σ relations are used. Adopting relations from the literature, we find that the M BH –σ relation yields an estimate of the total mass density in black holes that is roughly 55 per cent larger than if the M BH – M Bulge relation is used. 相似文献
13.
S. C. Chapman † C. M. Casey 《Monthly notices of the Royal Astronomical Society》2009,398(4):1615-1620
We present confusion-limited submillimetre (submm) observations with the Submillimetre Common-User Bolometer Array (SCUBA) camera on the James Clerk Maxwell Telescope of the z = 2.83 Lyman-break galaxy (LBG), Westphal–MM8, reaching an 850 μm sensitivity even greater than that achieved in the SCUBA map of the Hubble Deep Field region. The detection of MM8 ( S 850 μm = 1.98 ± 0.48 mJy) , along with the literature submm detections of lensed LBGs, suggests that the LBG population may contribute significantly to the source counts of submm-selected galaxies in the 1–2 mJy regime. Additionally, submm-luminous LBGs are a viable progenitor population for the recently discovered evolved galaxies at z ∼ 2–2.5 . These observations represent an important baseline for SCUBA2 observations which will regularly map large regions of the sky to this depth. 相似文献
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M. Nonino J. P. Henry C. Fanti R. Fanti & J. Davies 《Monthly notices of the Royal Astronomical Society》1998,299(2):332-340
We report on new optical, infrared and radio observations of the Seyfert galaxy Markarian 315. We confirm the detection at all wavelengths of a secondary peak of emission, which lies ≈ 2 arcsec east of the Seyfert nucleus. Moreover, we detect a chain-like structure which surrounds the active nucleus, with peculiar behaviour westward of the nucleus. We consider different interpretations for the origin of the secondary peak emission. 相似文献
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D. Michielsen A. Boselli C. J. Conselice E. Toloba I. M. Whiley A. Aragón-Salamanca M. Balcells N. Cardiel A. J. Cenarro J. Gorgas R. F. Peletier A. Vazdekis 《Monthly notices of the Royal Astronomical Society》2008,385(3):1374-1392
Dwarf galaxies, as the most numerous type of galaxy, offer the potential to study galaxy formation and evolution in detail in the nearby universe. Although they seem to be simple systems at first view, they remain poorly understood. In an attempt to alleviate this situation, the MAGPOP EU Research and Training Network embarked on a study of dwarf galaxies named MAGPOP-ITP. In this paper, we present the analysis of a sample of 24 dwarf elliptical galaxies (dEs) in the Virgo cluster and in the field, using optical long-slit spectroscopy. We examine their stellar populations in combination with their light distribution and environment. We confirm and strengthen previous results that dEs are, on average, younger and more metal-poor than normal elliptical galaxies, and that their [α/Fe] abundance ratios scatter around solar. This is in accordance with the downsizing picture of galaxy formation where mass is the main driver for the star formation history. We also find new correlations between the luminosity-weighted mean age, the large-scale asymmetry, and the projected Virgocentric distance. We find that environment plays an important role in the termination of the star formation activity by ram-pressure stripping of the gas in short time-scales, and in the transformation of discy dwarfs to more spheroidal objects by harassment over longer time-scales. This points towards a continuing infalling scenario for the evolution of dEs. 相似文献