1,446 research outputs found
Trithorax group proteins: switching genes on and keeping them active
Cellular memory is provided by two counteracting groups of chromatin proteins termed Trithorax group (TrxG) and Polycomb group (PcG) proteins. TrxG proteins activate transcription and are perhaps best known because of the involvement of the TrxG protein MLL in leukaemia. However, in terms of molecular analysis, they have lived in the shadow of their more famous counterparts, the PcG proteins. Recent advances have improved our understanding of TrxG protein function and demonstrated that the heterogeneous group of TrxG proteins is of critical importance in the epigenetic regulation of the cell cycle, senescence, DNA damage and stem cell biology
The Association of Compact Groups of Galaxies with Large-scale Structures
We use various samples of compact groups (CGs) to examine the types of
association CGs have with rich and poor clusters of galaxies at low (z~0.04)
and intermediate (z~0.1) redshifts. We find that ~10-20 % of CGs are associated
with rich clusters and a much larger fraction with poorer clusters or loose
groups. Considering the incompleteness of catalogs of poorer systems at
intermediate redshift, our result is consistent with all CGs at intermediate
redshift being associated with larger-scale systems. The richness of the
clusters associated with CGs significantly increases from z~0.04 to z~0.1,
while their Bautz-Morgan type changes from early to late type for the same
range in z. Neither trend is compatible with a selection effect in the cluster
catalogs used. We find earlier morphological types of galaxies to be more
frequent in CGs associated with larger-scale structures, compared to those in
CGs not associated to such structures. We consider this as new evidence that
CGs are part of the large-scale structure formation process and that they may
play an important role in the evolution of galaxies in these structures.Comment: 5 pages, no figures, Proc. ESO Workshop "Groups of galaxies in the
nearby Universe", Santiago, Chile, 5-9 Dec. 2005, ESO Astrophysics Symposia,
eds. I. Saviane, V. Ivanov & J. Borissova, Springer-Verlag; very minor
revision of text on 15 Mar 2006, added one referenc
Spectroscopy of the optical Einstein ring 0047-2808
We present optical and near-infrared spectroscopic observations of the
optical Einstein ring 0047-2808. We detect both [OIII] lines 4959, 5007 near
2.3 micron, confirming the redshift of the lensed source as z=3.595. The Ly-a
line is redshifted relative to the [OIII] line by 140+-20 km/s. Similar
velocity shifts have been seen in nearby starburst galaxies. The [OIII] line is
very narrow, 130 km/s FWHM. If the ring is the image of the centre of a galaxy
the one-dimensional stellar velocity dispersion sigma=55 km/s is considerably
smaller than the value predicted by Baugh et al. (1998) for the somewhat
brighter Lyman-break galaxies. The Ly-a line is significantly broader than the
[OIII] line, probably due to resonant scattering. The stellar central velocity
dispersion of the early-type deflector galaxy at z=0.485 is 250+-30 km/s. This
value is in good agreement both with the value predicted from the radius of the
Einstein ring (and a singular isothermal sphere model for the deflector), and
the value estimated from the D_n-sigma relation.Comment: 7 pages, 3 figures, accepted for publication in MNRA
Redshift-Space Distortions and the Real-Space Clustering of Different Galaxy Types
We study the distortions induced by peculiar velocities on the redshift-space
correlation function of galaxies of different morphological types in the
Pisces-Perseus redshift survey. Redshift-space distortions affect early- and
late-type galaxies in different ways. In particular, at small separations, the
dominant effect comes from virialized cluster cores, where ellipticals are the
dominant population. The net result is that a meaningful comparison of the
clustering strength of different morphological types can be performed only in
real space, i.e., after projecting out the redshift distortions on the
two-point correlation function xi(r_p,pi). A power-law fit to the projected
function w_p(r_p) on scales smaller than 10/h Mpc gives r_o =
8.35_{-0.76}^{+0.75} /h Mpc, \gamma = 2.05_{-0.08}^{+0.10} for the early-type
population, and r_o = 5.55_{-0.45}^{+0.40} /h Mpc, \gamma =
1.73_{-0.08}^{+0.07} for spirals and irregulars. These values are derived for a
sample luminosity brighter than M_{Zw} = -19.5. We detect a 25% increase of r_o
with luminosity for all types combined, from M_{Zw} = -19 to -20. In the
framework of a simple stable-clustering model for the mean streaming of pairs,
we estimate sigma_12(1), the one-dimensional pairwise velocity dispersion
between 0 and 1 /h Mpc, to be 865^{+250}_{-165} km/s for early-type galaxies
and 345^{+95}_{-65} km/s for late types. This latter value should be a fair
estimate of the pairwise dispersion for ``field'' galaxies; it is stable with
respect to the presence or absence of clusters in the sample, and is consistent
with the values found for non-cluster galaxies and IRAS galaxies at similar
separations.Comment: 17 LaTeX pages including 3 tables, plus 11 PS figures. Uses AASTeX
macro package (aaspp4.sty) and epsf.sty. To appear on ApJ, 489, Nov 199
The DPOSS II distant compact group survey: the EMMI-NTT spectroscopic sample
This paper presents the results of the redshift survey of 138 candidate
compact groups from the DPOSS II catalog (Iovino et al., 2003; de Carvalho et
al. 2005), which extends the available redshift range of spectroscopically
confirmed compact groups of galaxies to z~0.2. The aims of the survey are to
confirm group membership via spectroscopic redshift information, to measure the
characteristic parameters of the confirmed groups, namely mass, radius,
luminosity, velocity dispersion and crossing time, and to compare them with
those of nearby compact groups. Using available information from the
literature, we also studied the surrounding group environment and searched for
additional, previously unknown, group members, or larger scale structures to
whom the group might be associated. Of the 138 observed groups, 96 had three or
more concordant galaxies, i.e. a 70% success rate. Of these 96, 62 are isolated
on the sky, while the other 34 are close on the sky to a larger scale
structure. The remaining objects turned out to be couple of pairs or chance
projection of galaxies on the sky. Group environment and the characteristics
parameters (mass, crossing time, velocity dispersion) are evaluated and
discussed.Comment: Accepted on A&A, version updated to match the printed one. The paper
will read well even without printing figures 8 and
Dust Absorption and the Cosmic UV Flux Density
We study the evolution of the galaxy UV luminosity density as a function of
redshift in the Hubble Deep Field North (HDF-N). We estimate the amount of
energy absorbed by dust and hidden from optical observations by analyzing the
HDF-N photometric data with the spectral energy distribution fitting method.
According to our results, at redshifts 1 < z < 4.5, the global energy observed
in the UV rest-frame at lambda=1500 A corresponds to only 7-11% of the stellar
energy output, the rest of it being absorbed by dust and re-emitted in the
far-IR. Our estimates of the comoving star formation rate density in the
universe from the extinction-corrected UV emission are consistent with the
recent results obtained with Submillimeter Common-User Bolometer Array
(SCUBA) at faint sub-millimeter flux levels.Comment: 14 pages, 3 encapsulated postscript figures, LateX, accepted for
publication in ApJ
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