187 research outputs found
Software and Sociology in UK Astronomy
I discuss the remit of Starlink's software strategy groups and a particular
item on the agenda of a meeting of the image processing software strategy group
held on 26th January 2001: `Why don't people use Starlink software?'. The
answer to this question was speculated to be primarily a sociological effect:
those people supervising UK astronomy Ph.D. students are largely people who had
learnt their trade at a time when Starlink had a less than perfect reputation.
I report on the recommendations made to Starlink to counter this effect.Comment: 3 pages. Accepted for publication in Astronomy & Geophysics (formerly
QJRAS
Pulling out Threads from the Cosmic Tapestry: Defining Filaments of Galaxies
Filaments of galaxies are the dominant feature of modern large scale redshift
surveys. They can account for up to perhaps half of the baryonic mass budget of
the Universe and their distribution and abundance can help constrain
cosmological models. However, there remains no single, definitive way in which
to detect, describe and define what filaments are and their extent. This work
examines a number of physically motivated, as well as statistical, methods that
can be used to define filaments and examines their relative merits.Comment: 12 pages, 6 figures, accepted for publication in PAS
Stellar populations of X-Ray luminous clusters at z = 0.1
This thesis presents new and unique wide-field imaging and spectroscopic observations of 21 X-ray selected rich clusters of galaxies in the redshift range 0.07 < z < 0.16 from the Las Campanas Observatory (LCO) / Anglo-Australian Telescope (AAT) Rich Cluster Survey (LARCS). Mosaic two colour broad-band CCD imaging extending to 10 Mpc at the mean redshift of the survey have been taken at LCO; comprising over 50Gb of raw data. A reduction pipeline is developed for these data and catalogues are constructed for these clusters. Four of these fields are compared to the APM catalogue (Maddox et al. 1990) to confirm their photometric accuracy. In making the comparison several populations of galaxies are discovered to be absent from the APM.A statistical background correction technique is developed to examine the photometric properties of cluster members. Eleven clusters are combined together to investigate environmental trends in the stellar populations of the combined sample. It is found that the modal colours of galaxies lying on the colour-magnitude relation in the clusters become bluer by d (B - R)/dr(_p) = -0.022 ±0.004 with radius or d (B - R)/dlog(_10) (Σ) = -0.076 ± 0.009 with local galaxy density. The 2dF spectroscope at the A AT is used to make spectroscopic follow-up observations of three clusters. A reduction pipeline for these data is developed and redshifts for the galaxies are determined. The spectral catalogues are used to define cluster membership and confirm the photometric environmental trends. Spectral line strengths are used to classify the galaxy population and examine environmental trends across the clusters. The cluster cores are found to be predominantly passive compared to the field. A comparison of the two cluster membership assignment techniques underscores the need for spectroscopy to define the cluster population
The h-index in Australian Astronomy
The Hirsch (2005) h-index is now widely used as a metric to compare
individual researchers. To evaluate it in the context of Australian Astronomy,
the h-index for every member of the Astronomical Society of Australia (ASA) is
found using NASA's Astrophysics Data System Bibliographic Services (ADS).
Percentiles of the h-index distribution are detailed for a variety of
categories of ASA members, including students. This enables a list of the top
ten Australian researchers by h-index to be produced. These top researchers
have h-index values in the range 53<h<77, which is less than that recently
reported for the American Astronomical Society Membership. We suggest that
membership of extremely large consortia such as SDSS may partially explain the
difference. We further suggest that many student ASA members with large h-index
values have probably already received their Ph.D.'s and need to upgrade their
ASA membership status. To attempt to specify the h-index distribution relative
to opportunity, we also detail the percentiles of its distribution by years
since Ph.D. award date. This shows a steady increase in h-index with seniority,
as can be expected.Comment: Accepted for publication in the Publications of the Astronomical
Society of Australi
The Large Peculiar Velocity of the cD Galaxy in Abell 3653
We present a catalogue of galaxies in Abell 3653 from observations made with
the 2dF spectrograph at the Anglo-Australian Telescope. Of the 391 objects
observed, we find 111 are bone-fide members of Abell 3653. We show that the
cluster has a velocity of cz = 32214 +/- 83 km/s (z=0.10738 +/- 0.00027), with
a velocity dispersion typical of rich, massive clusters of sigma_{cz} =
880^{+66}_{-54}. We find that the cD galaxy has a peculiar velocity of 683 +/-
96 km/s in the cluster restframe - some 7sigma away from the mean cluster
velocity, making it one of the largest and most significant peculiar velocities
found for a cD galaxy to date. We investigate the cluster for signs of
substructure, but do not find any significant groupings on any length scale. We
consider the implications of our findings on cD formation theories.Comment: 16 pages, including 7 figures and a long table. Accepted for
publication in MNRA
The Rarity of Star Formation in Brightest Cluster Galaxies as Measured by WISE
We present the mid-infrared (IR) star formation rates of 245 X-ray selected,
nearby (z<0.1) brightest cluster galaxies (BCGs). A homogeneous and volume
limited sample of BCGs was created by X-ray selecting clusters with L_x >
1x10^44 erg/s. The Wide-Field Infrared Survey Explorer (WISE) AllWISE Data
Release provides the first measurement of the 12 micron star formation
indicator for all BCGs in the nearby Universe. Perseus A and Cygnus A are the
only galaxies in our sample to have star formation rates of > 40 M_sol/yr,
indicating that these two galaxies are highly unusual at current times. Stellar
populations of 99 +/- 0.6 % of local BCGs are (approximately) passively
evolving, with star formation rates of <10 M_sol/yr. We find that in general,
star formation produces only modest BCG growth at the current epoch.Comment: 5 pages, 3 figures, accepted for publication in MNRA
An accurate new method of calculating absolute magnitudes and K-corrections applied to the Sloan filter set
We describe an accurate new method for determining absolute magnitudes, and
hence also K-corrections, which is simpler than most previous methods, being
based on a quadratic function of just one suitably chosen observed color. The
method relies on the extensive and accurate new set of 129 empirical galaxy
template SEDs from Brown et al. (2014). A key advantage of our method is that
we can reliably estimate random errors in computed absolute magnitudes due to
galaxy diversity, photometric error and redshift error. We derive K-corrections
for the five Sloan Digital Sky Survey filters and provide parameter tables for
use by the astronomical community. Using the New York Value-Added Galaxy
Catalog we compare our K-corrections with those from kcorrect. Our
K-corrections produce absolute magnitudes that are generally in good agreement
with kcorrect. Absolute g, r, i, z-band magnitudes differ by less than 0.02
mag, and those in the u-band by ~0.04 mag. The evolution of rest-frame colors
as a function of redshift is better behaved using our method, with relatively
few galaxies being assigned anomalously red colors and a tight red sequence
being observed across the whole 0.0 < z < 0.5 redshift range.Comment: 23 pages, 16 figure
Multiscale probability mapping: groups, clusters and an algorithmic search for filaments in SDSS
We have developed a multiscale structure identification algorithm for the
detection of overdensities in galaxy data that identifies structures having
radii within a user-defined range. Our "multiscale probability mapping"
technique combines density estimation with a shape statistic to identify local
peaks in the density field. This technique takes advantage of a user-defined
range of scale sizes, which are used in constructing a coarse-grained map of
the underlying fine-grained galaxy distribution, from which overdense
structures are then identified. In this study we have compiled a catalogue of
groups and clusters at 0.025 < z < 0.24 based on the Sloan Digital Sky Survey,
Data Release 7, quantifying their significance and comparing with other
catalogues. Most measured velocity dispersions for these structures lie between
50 and 400 km/s. A clear trend of increasing velocity dispersion with radius
from 0.2 to 1 Mpc/h is detected, confirming the lack of a sharp division
between groups and clusters. A method for quantifying elongation is also
developed to measure the elongation of group and cluster environments. By using
our group and cluster catalogue as a coarse-grained representation of the
galaxy distribution for structure sizes of <~ 1 Mpc/h, we identify 53 filaments
(from an algorithmically-derived set of 100 candidates) as elongated unions of
groups and clusters at 0.025 < z < 0.13. These filaments have morphologies that
are consistent with previous samples studied.Comment: 22 pages, 14 figures and 6 tables. Accepted for publication in MNRAS.
Data products, three-dimensional visualisations and further information about
MSPM can be found at http://www.physics.usyd.edu.au/sifa/Main/MSPM/ . v2
contains two additional references. v3 has a slightly altered title and
updated reference
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