共查询到20条相似文献，搜索用时 31 毫秒
1.
H. J. Martínez † A. Zandivarez† M. Domínguez‡ M. E. Merchán† D. G. Lambas† 《Monthly notices of the Royal Astronomical Society》2002,333(2):L31-L34
We estimate the fraction of star-forming galaxies in a catalogue of groups, constructed from the 2dF Galaxy Redshift Survey by Merchán & Zandivarez. We use the η spectral type parameter of galaxies and subdivide the sample of galaxies in groups into four types depending on the values of the η parameter following Madgwick et al. We obtain a strong correlation between the relative fraction of galaxies with high star formation and the parent group virial mass. We find that even in the environment of groups with low virial mass M ∼1013 M⊙ the star formation of their member galaxies is significantly suppressed. The relation between the fraction of early-type galaxies and the group virial mass obeys a simple power law spanning over three orders of magnitude in virial mass. Our results show quantitatively the way that the presence of galaxies with high star formation rates is inhibited in massive galaxy systems. 相似文献
2.
We study the variations of the properties of groups of galaxies with dynamical masses of 1013 M ⊙<M 200<1014 M ⊙, represented by two samples: one has redshifts of z < 0.027 and is located in the vicinity of the Coma cluster, the other has z > 0.027, and is located in the regions of the following superclusters of galaxies: Hercules, Leo, Bootes, Ursa Major, and Corona Borealis. Using the archived data of the SDSS and 2MASX catalogs, we determined the concentration of galaxies in the systems by measuring it as the inner density of the group within the distance of the fifth closest galaxy from the center brighter than M K = ?23. m 3. We also measured the magnitude gap between the first and the fourth brightest galaxies ΔM 14 located within one half of the selected radius R 200, the fraction of early-type galaxies, and the ratio of bright dwarf galaxies (Mr = [?18. m 5,?16. m 5]) to giant galaxies (M r < ?18. m 5) (DGR) within the radius R 200. The main aim of the investigation is to find among these characteristics the ones that reflect the evolution of groups of galaxies.We determined that the ratio of bright dwarf galaxies to early-type giant galaxies on the red sequence depends only on the x-ray luminosity: the DGR increases with luminosity. The fraction of early-type galaxies in the considered systems is equal, on average, to 0.65 ± 0.01, and varies significantly for galaxies with σ200 < 300 kms?1. Based on the luminosity of the brightest galaxy, the magnitude gap between the first and the fourth brightest galaxies in the groups, and on model computations of these parameters, we selected four fossil group candidates: AWM4, NGC0533, NGC0741, and NGC6098 (where the brightest galaxy is a double).We observe no increase in the number of faint galaxies (the α parameter of the Schechter function is less than 1) in our composite luminosity function (LF) for galaxy systems with z < 0.027 in the M K = [?26m,?21. m 5] range, whereas earlier we obtained α > 1 for the LF of the Hercules and Leo superclusters of galaxies. 相似文献
3.
Peter Goldreich 《Astrophysics and Space Science》2001,278(1-2):17-23
The inertial range of incompressible MHD turbulence is most conveniently described in terms of counter propagating waves.
Shear Alfvén waves control the cascade dynamics. Slow waves play a passive role and adopt the spectrum set by the shear Alfvén
waves. Cascades composed entirely of shear Alfvén waves do not generate a significant measure of slow waves. MHD turbulence
is anisotropic with energy cascading more rapidly along k
⊥ than along k
∥. Anisotropy increases with k
⊥ such that the excited modes are confined inside a cone bounded by k
∥∝ k
perp
2/3. The opening angle of the cone, θ(k
⊥)∝ k
⊥
-1/3, defines the scale dependent anisotropy. MHD turbulence is generically strong in the sense that the waves which comprise
it are critically damped. Nevertheless, deep inside the inertial range, turbulent fluctuations are small. Their energy density
is less than that of the background field by a factor θ2(k
⊥)≪. MHD cascades are best understood geometrically. Wave packets suffer distortions as they move along magnetic field lines
perturbed by counter propagating wave packets. Field lines perturbed by unidirectional waves map planes perpendicular to the
local field into each other. Shear Alfvén waves are responsible for the mapping's shear and slow waves for its dilatation.
The former exceeds the latter by θ-1(k
⊥)≫ 1 which accounts for dominance of the shear Alfvén waves in controlling the cascade dynamics.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
4.
We analyze the properties of galaxy clusters in the region of the Leo supercluster using observational data from the SDSS
and 2MASS catalogs. We have selected 14 galaxy clusters with a total dynamical mass of 1.77 × 1015
M
⊙ in the supercluster region 130 by 60 Mpc in the plane of the sky (z ≃ 0.037). The composite luminosity function of the supercluster is described by a Schechter function with parameters that,
within the error limits, correspond to field galaxies and does not differ from the luminosity function of the richer Ursa
Major (UMa) supercluster for the same luminosity range (the bright end). The luminosity functions of early-type and late-type
galaxies in Leo at the faint end are characterized by a sharp decrease (α = −0.60±0.08) and a steep increase (α = −1.44± 0.10) in the number of galaxies, respectively. In the virialized cluster regions, the fraction of early-type galaxies
selected by the u-r color, bulge contribution, and concentration index among the galaxies brighter than M
K
* + 1 is, on average, 62%. This fraction is smaller than that in the UMa supercluster at a 2–3σ level. The near-infrared luminosities of galaxy clusters down to a fixed absolute magnitude correlate with their masses almost
in the same way as for other samples of galaxy clusters (L
200,K
∝ M
2000.63±0.11)). 相似文献
5.
We study the A1831 cluster within the framework of our program of the investigation of galaxy clusters with bimodal velocity
distributions (i.e., clusters where the velocities of subsystems differ by more than Δ
cz
∼ 3000 km/s).We identify two subsystems in this cluster: A1831A (cz = 18970 km/s) and A1831B (cz = 22629 km/s) and directly estimate the distances to these subsystems using three methods applied to early-type galaxies:
the Kormendy relation, the photometric plane, and the fundamental plane. To this end, we use the results of our observations
made with the 1-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences and the data adopted
from the SDSS DR6 catalog. We confirmed at a 99% confidence level that (1) the two subsystems are located at different distances,
which are close to their Hubble distances, and (2) the two subsystems are located behind one another along the line of sight
and are not gravitationally bound to each other. Both clusters have a complex internal structure, which makes it difficult
to determine their dynamical parameters. Our estimates for the velocity dispersions and masses of the two clusters: 480 km/s
and 1.9 × 1014
M
⊙ for A1831A, 952 km/s and 1.4 × 1015
M
⊙ for A1831B should be views as upper limits. At least three spatially and kinematically distinct groups of galaxies can be
identified in the foreground cluster A1831A, and this fact is indicative of its incomplete dynamical relaxation. Neither can
we rule out the possibility of a random projection. The estimate of the mass of the main cluster A1831B based on the dispersion
of the line-of-sight velocities of galaxies is two-to-three times greater than the independent mass estimates based on the
total K-band luminosity, temperature, and luminosity of the X-ray gas of the cluster. This fact, combined with the peculiarities
of its kinematical structure, leads us to conclude that the cluster is in a dynamically active state: galaxies and groups
of galaxies with large line-of-sight velocities relative to the center of the cluster accrete onto the virialized nucleus
of the cluster (possibly, along the filament directed close to the line of sight). 相似文献
6.
We investigate the distribution and velocity field of galaxies situated in a band of 100 by 20 degrees centered on M87 and oriented along the Local supercluster plane. Our sample amounts 2158 galaxies with radial velocities less than 2000 km s?1. Of them, 1119 galaxies (52%) have distance and peculiar velocity estimates. About 3/4 of early-type galaxies are concentrated within the Virgo cluster core, most of the late-type galaxies in the band locate outside the virial radius. Distribution of gas-rich dwarfs with MHI >M* looks to be insensitive to the Virgo cluster presence. Among 50 galaxy groups in the equatorial supercluster band 6 groups have peculiar velocities about 500–1000 km s?1 comparable with virial motions in rich clusters. The most cryptic case is a flock of nearly 30 galaxies around NGC4278 (Coma I cloud), moving to us with the mean peculiar velocity of ?840 km s?1. This cloud (or filament?) resides at a distance of 16.1 Mpc from us and approximately 5 Mpc away from the Virgo center. Galaxies around Virgo cluster exhibit Virgocentric infall with an amplitude of about 500 km s?1. Assuming the spherically symmetric radial infall, we estimate the radius of the zero-velocity surface to be R0 = (7.0±0.3) Mpc that yields the total mass of Virgo cluster to be (7.4 ± 0.9)× 1014M⊙ in tight agreement with its virial mass estimates. We conclude that the Virgo outskirts does not contain significant amounts of dark mater beyond its virial core. 相似文献
7.
We present the results of our stellar photometry and spectroscopy for the new Local Group galaxy VV124 (UGC4879) obtainedwith
the 6-m BTAtelescope. The presence of a fewbright supergiants in the galaxy indicates that the current star formation process
is weak. The apparent distribution of stars with different ages in VV 124 does not differ from the analogous distributions
of stars in irregular galaxies, but the ratio of the numbers of young and old stars indicates that VV 124 belongs to the rare
Irr/Sph type of galaxies. The old stars (red giants) form the most extended structure, a thick disk with an exponential decrease
in the star number density to the edge. Definitely, the young population unresolvable in images makes a great contribution
to the background emission from the central galactic regions. The presence of young stars is also confirmed by the [OIII]
emission line visible in the spectra that belongs to extensive diffuse galactic regions. The mean radial velocity of several
components (two bright supergiants, the unresolvable stellar population, and the diffuse gas) is υ
h = −70 ± 15 km s−1 and the velocity with which VV 124 falls into the Local Group is υ
LG = −12 ± 15 km s−1. We confirm the distance to the galaxy (D = 1.1 ± 0.1 Mpc) and the metallicity of red giants ([Fe/H] = −1.37) found by Kopylov et al. (2008). VV 124 is located on
the periphery of the Local Group approximately at the same distance from M31 and our Galaxy and is isolated from other galaxies.
The galaxy LeoA nearest to it is 0.5 Mpc away. 相似文献
8.
The observed relationship between stellar mass and effective radius for early type galaxies, pointed out by many authors, is interpreted in the context of Clausius’ virial maximum theory. In this view, it is strongly underlined that the key of the above mentioned correlation is owing to the presence of a deep link between cosmology and the existence of the galaxy Fundamental Plane. Then the ultimate meaning is: understanding visible mass-size correlation and/or Fundamental Plane means understanding how galaxies form. The mass-size relationship involves baryon (mainly stellar) mass and its typical dimension related to the light, but it gets memory of the cosmological mass variance at the equivalence epoch. The reason is that the baryonic component virializes by sharing virial energy in about equal amount between baryons and dark matter, this sharing depending, in turn, on the steepness of the dark matter distribution. The general strategy consists in using the two-component tensor virial theorem for determining the virialized baryonic configurations. A King and a Zhao density profile are assumed for the inner baryonic and the outer dark matter component, respectively, at the end of the relaxation phase. All the considerations are restricted to spherical symmetry for simplicity. The effect of changing the dark-to-baryon mass ratio, m, is investigated inside a ΛCDM scenario. A theoretical mass-size relation is expressed for the baryonic component, which fits fairly well to the data from a recently studied galaxy sample. Finally, the play of intrinsic dispersion on the mass ratio, m, is discussed in the light of the cusp/core problem and some consequences are speculated about the existence of a limit ml expected by the theory. 相似文献
9.
A. V. Tikhonov 《Astronomy Letters》2007,33(8):499-511
Using the method of searching for arbitrary shaped voids in the distribution of volume-limited samples of galaxies from the DR5 SDSS survey, we have identified voids and investigated their characteristics and the change in these characteristics with decreasing M lim (from ?19.7 to ?21.2, H 0 = 100 km s?1 Mpc?1)—the upper limit on the absolute magnitude of the galaxies involved in the construction of voids. The total volume of the 50 largest voids increases with decreasing M lim with a break near M* = ?20.44—the characteristic value of the luminosity function for SDSS galaxies. The mean overdensity in voids increases with decreasing M lim also with a weak break near M*. The exponent of the dependence of the volume of a void on its rank increases significantly with decreasing M lim starting from M lim ～ ?20.4 in the characteristic range of volumes, which reflects the tendency for greater clustering of brighter galaxies. The averaged profile of the galaxy overdensity in voids has a similar pattern almost at all M lim. The galaxies mostly tend to gravitate toward the void boundaries and to avoid the central void regions; the overdensity profile is flat in the intermediate range of distances from the void boundaries. The axial ratios of the ellipsoids equivalent to the voids are, on average, retained with changing M lim and correspond to elongated and nonoblate void shapes, but some of the voids can change their shape significantly. The directions of the greatest void elongations change chaotically and are distributed randomly at a given M lim. The void centers show correlations reflecting the correlations of the galaxy distribution on scales (35–70)h ?1 Mpc. The galaxy distribution in the identified voids is nonrandom—groups and filaments can be identified. We have compared the properties of the galaxies in voids (in our case, the voids are determined by the galaxies with absolute magnitudes M abs < M lim = ?20.44, except for the isolated galaxies) and galaxies in structures identified using the minimum spanning tree. A bimodal color distribution of the galaxies in voids has been obtained. A noticeable difference is observed in the mean color indices and star formation rates per unit stellar mass of the galaxies in dense regions (structures)—as expected, the galaxies in voids are, on average, bluer and have higher log (SFR/M star). These tendencies become stronger toward the central void regions. 相似文献
10.
In this paper we study the relations between the main characteristics of groups and clusters of galaxies using the archival data of the SDSS and 2MASX catalogs. We have developed and implemented a new method of determining the size of galaxy systems and their effective radius which contains half of the galaxies and not half the luminosity, since the luminosity of the brightest galaxy in a group can account for over 50% of the total luminosity of the group. The derived parameters (log LK, logRe, and log σ200) for 94 systems of galaxies (0.0038 < z < 0.09) determine the Fundamental Plane (FP), which, with a scatter of 0.15, is similar in form to the FP of galaxy clusters obtained by Schaeffer et al. (1993) and D’Onofrio et al. (2013) with other methods and for different bands. We show that the FP in the near-infrared region (NIR) for 94 galaxy systems has the form of LK ∝ \(R_e^{0.70 \pm {{0.13}_\sigma }1.34 \pm 0.13}\), whereas in x-rays it has the form of—LX ∝ \(R_e^{1.15 \pm {{0.39}_\sigma }2.56 \pm 0.40}\). The form of the FP for groups and clusters is consistent with the FP for early-type galaxies determined in the same way. The form of the FP for galaxy systems deviates from the shape that one would expect from virial predictions. Adding the mass-to-light ratio as a fourth independent parameter has little effect on this deviation, but decreases the scatter of the FP for a sample of rich galaxy clusters by 12%. 相似文献
11.
Based on high precision measurements of the distances to nearby galaxies with the Hubble telescope, we have determined the
radii of the zero velocity spheres for the local group, R0 = 0.96±0.03Mpc, and for the group of galaxies around M 81/M 82, 0.89±0.05Mpc. These yield estimates of MT = (1.29±0.14)· 1012 M⊙ and (1.03±0.17)· 1012 M⊙, respectively, for the total masses of these groups. The R0 method allows us to determine the mass ratios for the two brightest members in both groups, as well. By varying the position
of the center of mass between the two principal members of a group to obtain minimal scatter in the galaxies on a Hubble diagram,
we find mass ratios of 0.8:1.0 for our galaxy and Andromeda and 0.54:1.00 for the M82 and M81 galaxies, in good agreement
with the observed ratios of the luminosities of these galaxies.
__________
Translated from Astrofizika, Vol. 49, No. 1, pp. 5–22 (February 2006). 相似文献
12.
We have performed a series ofN-body experiments including the effects of a massive dominant background which follows Schuster's density law in order to simulate clusters of galaxies in which a smoothly distributed dark component is present. The existence of this background is inferred from the weak luminosity segregation observed in clusters which, however, show several characteristics of well-relaxed systems. The comparison of the velocity dispersion profiles of three clusters of galaxies (Coma, Perseus, and Virgo) with those obtained in the numerical experiments allows us to place some constraints on both the distribution and amount of distributed dark material in these clusters. The profiles are rather insensitive to variations in the ratio of the background mass to the mass attached to galaxies (M
b/Mg), but exhibit a strong dependence on their relative concentration. We conclude that highly concentrated background models are not consistent with observations. We find a maximum value for the ratio of the gravitational radius of the galaxies and the background (R
g/Rb) (approximately 0.6) and using previous results (Navarroet al., 1986) we conclude that virial theorem masses underestimate the total mass (M
b+M
g) of the clusters. As a final result, we derive a minimum value for theM
b/Mg ratio. All these conclusions could apply in general if Coma, Perseus, and Virgo constitute a fair sample of the rich clusters of galaxies in the Universe. 相似文献
13.
We have obtained Hα fluxes and luminosities for a sample of 95 galaxies from observations of 31 Hickson Compact Groups (HCGs) in the northern
hemisphere. This sample is the largest Hα selected catalogue of galaxies having Hα calibrated fluxes so far. The results obtained from a preliminary analysis of a subsample of66 galaxies show that the Hα luminosity of the galaxies is correlated with velocity dispersion and compactness of groups. These correlations would point
towards a scenario in which the brightest Hα galaxies reside in compact groups having higher probability of galaxy interaction, i.e. lower values of velocity dispersion.
Moreover, such relations seem to depend on the environment in which HCGs themselves are embedded.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
14.
J. R. Martirosian 《Astrophysics》2007,50(3):301-310
This is a statistical study of galaxies with a UV excess. A sample of 702 Kazarian galaxies (KG) is used. The KGs are identified
with objects from the MAPS, IRAS FSC, IRAS PSC, and NVSS catalogs. The O and E magnitudes are known for more than 92% of the
KGs. It is shown that the KG sample is complete up to 16m.0 in the blue and to 16m.5 in the red. More than 36% of the KGs
are identified with infrared (IR) sources at wavelengths of 12, 25, 60, and 100 m. Calculations of the far IR (FIR) luminosities
show that 4% of the KGs are strong FIR emitters (LFIR ≥ 1011 L⊙). More than 32% of the KGs have been identified as radio sources at a frequency of 1.4 GHz. A determination of the radio
luminosities shows that the sample of KGs with known radial velocities include one powerful, LR ≥ 1025 W/Hz, radio object (Kaz 273) which is a BL Lac object. A close correlation (r=0.93) is bound between the FIR and radio luminosities
for galaxies with a UV excess. An examination of the relationship between the FIR and radio luminosities for galaxies in different
spectral classes shows that the correlation coefficient is higher (r=0.99) and the slope of the fit curve is larger (a=1.18)
for Seyfert galaxies. Calculations of the logarithm of the ratio of the FIR and radio fluxes indicate that the sample includes
4 KGs with a radio excess, while there are none with an IR excess.
__________
Translated from Astrofizika, Vol. 50, No. 3, pp. 369–379 (August 2007). 相似文献
15.
16.
Electromagnetic instabilities in high-β plasmas, where β is the ratio of the kinetic plasma energy to the magnetic energy, have a broad range of astrophysical applications. The presence
of temperature anisotropies T
∥
/T
⊥
>1 (where ∥ and ⊥ denote directions relative to the background magnetic field) in solar flares and the solar wind is sustained by the observations
and robust acceleration mechanisms that heat plasma particles in the parallel direction. The surplus of parallel kinetic energy
can excite either the Weibel-like instability (WI) of the ordinary mode perpendicular to the magnetic field or the firehose
instability (FHI) of the circularly polarized waves at parallel propagation. The interplay of these two instabilities is examined.
The growth rates and the thresholds provided by the kinetic Vlasov – Maxwell theory are compared. The WI is the fastest growing
one with a growth rate that is several orders of magnitude larger than that of the FHI. These instabilities are however inhibited
by the ambient magnetic field by introducing a temperature anisotropy threshold. The WI admits a larger anisotropy threshold,
so that, under this threshold, the FHI remains the principal mechanism of relaxation. The criteria provided here by describing
the interplay of the WI and FHI are relevant for the existence of these two instabilities in any space plasma system characterized
by an excess of parallel kinetic energy. 相似文献
17.
In order to compare color statistical properties of member galaxies in compact groups with those of field galaxies, we use
a compact group (CG) sample which contains 4217 CGs extracted from the MAIN galaxy sample of the SDSS Data Release 4 (SDSS4),
and construct a random group sample which has the same distributions of redshift and number of member galaxies as those of
the CG sample. It turns out that the mean colors of galaxies in CGs are redder than those of galaxies in random groups. Additionally,
we also find that member galaxies in real CGs have a smaller dispersion of colors than those in random groups-at least for
g-r, r-i, and i-z colors.
Published in Astrofizika, Vol. 50, No. 1, pp. 29–37 (February 2007). 相似文献
18.
A. M. Mel’nik 《Astronomy Letters》2006,32(1):7-13
The kinematics of the Sagittarius (R = 5.7 kpc),Carina (R = 6.5 kpc), Cygnus (R = 6.8 kpc), and Perseus (R = 8.2 kpc) arms suggests the existence of two spiral patterns in the Galaxy that rotate with different speeds. The inner
spiral pattern that is represented by the Sagittarius arm rotates with the speed of the bar, Ωb = 60 ± 5 km s−1 kpc−1, while the outer spiral pattern that includes the Carina, Cygnus, and Perseus arms rotates with a lower speed, Ωs = 12–22 km s−1 kpc−1.The existence of an outer slow tightly wound spiral pattern and an inner fast spiral pattern can be explained by numerically
simulating the dynamics of outer pseudorings. The outer Lindblad resonance of the bar must be located between the Sagittarius
and Carina arms. The Cygnus arm appears as a connecting link between the fast and slow spiral patterns. 相似文献
19.
We have derived the galaxy luminosity function in various regions of the cluster of galaxies Abell 496 from a wide field image
in the I band. A Schechter function fit in the 17≤ IAB ≤22(–19.5≤ MIAB ≤ –14.5) magnitude interval gives a steep power law index, which is somewhat steeper in the outer regions than in the inner
zones. This result agrees with previous findings obtained by several teams on the Coma cluster and can be interpreted as due
to the fact that faint galaxies are accreted by large ones in the central regions.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献
20.
Maite Rozas Almudena Zurita John E. Beckmann/snm> 《Astrophysics and Space Science》2001,276(2-4):1179-1188
We combine Hα and broad-band optical imaging and Hα velocity mapping over the face of the barred galaxy NGC 3359, obtained within the BARS programme on the Canary Island telescopes
(Lourenso and Beckman, these proceedings).From the Hα image we have determined the positions, fluxes and diameters of a total of 547 HII regions, and computed their luminosity
function whose slope is within the range of those of morphologically similar galaxies found in the literature. We have gone
on to quantify other statistical properties, such as the diameter distribution and the flux densities of the regions. Using
Fabry-Perot mapping in Hα with the TAURUS II instrument, we have produced maps of velocity and velocity dispersion, and computed the rotation curve
out to ∼ 3 scale lengths from the centre of the galaxy. From the map of the residual velocities we detected streaming motions
in the gas across the spiral arms and the presence of non-circular motions of order 30–40 km s-1 around the bar: the gas response to the gravitational potential.
This revised version was published online in July 2006 with corrections to the Cover Date. 相似文献