3,738 research outputs found
The HI gas content of galaxies around Abell 370, a galaxy cluster at z = 0.37
We used observations from the Giant Metrewave Radio Telescope to measure the
atomic hydrogen gas content of 324 galaxies around the galaxy cluster Abell 370
at a redshift of z = 0.37 (a look-back time of ~4 billion years). The HI 21-cm
emission from these galaxies was measured by coadding their signals using
precise optical redshifts obtained with the Anglo-Australian Telescope. The
average HI mass measured for all 324 galaxies is (6.6 +- 3.5)x10^9 solar
masses, while the average HI mass measured for the 105 optically blue galaxies
is (19.0 +- 6.5)x10^9 solar masses. The significant quantities of gas found
around Abell 370, suggest that there has been substantial evolution in the gas
content of galaxy clusters since redshift z = 0.37. The total amount of HI gas
found around Abell 370 is up to ~8 times more than that seen around the Coma
cluster, a nearby galaxy cluster of similar size. Despite this higher gas
content, Abell 370 shows the same trend as nearby clusters, that galaxies close
to the cluster core have lower HI gas content than galaxies further away. The
Abell 370 galaxies have HI mass to optical light ratios similar to local galaxy
samples and have the same correlation between their star formation rate and HI
mass as found in nearby galaxies. The average star formation rate derived from
[OII] emission and from de-redshifted 1.4 GHz radio continuum for the Abell 370
galaxies also follows the correlation found in the local universe. The large
amounts of HI gas found around the cluster can easily be consumed by the
observed star formation rate in the galaxies over the ~4 billion years (from z
= 0.37) to the present day.Comment: accepted by MNRA
The Mount Stromlo Abell Cluster Supernova Search
We have initiated a three-year project to find supernovae (SNe) in a
well-defined sample of high-density southern Abell clusters with redshifts
. These observations will provide a volume-limited sample of SNe Ia
to more than a magnitude below their peak brightness, and will enable us to:
(1) measure the luminosity function of SNe, (2) further explore the correlation
of light curve shape with the absolute luminosity of SNe Ia to better
understand SNe Ia as distance indicators, (3) measure SN rates, (4) measure the
bulk motion of the Local Group using SNe Ia, and (5) directly compare SN Ia
distances to brightest cluster galaxy distances. We use the MaCHO wide-field
2-color imager on the 1.3m telescope at Mount Stromlo to routinely monitor
clusters per week. We describe our technique for target selection and
scheduling search observations, and for finding and identifying SN candidates.
We also describe the results from the first year of our program, including the
detection of 19 SNe, several RR-Lyrae variables, and hundreds of asteroids.Comment: 20 pages, 10 figures, 3 tables. Accepted for publication in AJ, Jan.
1998 issu
An Experimental Examination of Activist Type and Effort on Brand Image and Purchase Intentions
In 2016, several prominent athletes kneeled or sat during the national anthem of their games to protest
social injustice in America. For their activism, these athletes inconsistently experienced both positive and
negative consequences from their sponsors and fans. Therefore, the purpose of this study was to investigate
this phenomenon more closely by examining the effect of activism type and activism effort on a sponsor’s
brand image and purchase intention of a product the athlete endorses, when controlling for brand familiarity.
Participants (N = 384) were randomly assigned into groups in a 2 (activism type: safe, risky) x 2
(activism effort: low, high) experimental study. Results indicated brand image and purchase intention were
negatively impacted by risky activism compared to safe activism, but activism effort had no effect on the
two variables. Further implications and future research are expanded upon in the discussion
SN1997cy/GRB970514 - A New Piece in the GRB Puzzle?
We present observations of SN1997cy, a supernova discovered as part of the
Mount Stromlo Abell Cluster SN Search, which does not easily fit into the
traditional classification scheme for supernovae. This object's extraordinary
optical properties and coincidence with GRB970514, a short duration gamma ray
burst, suggest a second case, after SN1998bw/GRB980425, for a SN-GRB
association. SN1997cy is among the most luminous SNe yet discovered and has a
peculiar spectrum. We present evidence that SN1997cy ejected approximately 2
solar masses of 56Ni, supported by its late-time light curve, and FeII/[FeIII]
lines in its spectrum, although it is possible that both these observations can
be explained via circumstellar interaction. While SN1998bw and SN1997cy appear
to be very different objects with respect to both their gamma ray and optical
properties, SN1997cy and the optical transient associated with GRB970508 have
roughly similar late-time optical behavior. This similarity may indicate that
the late-time optical output of these two intrinsically bright transient events
have a common physical process. Although the connection between GRB970514 and
SN1997cy is suggestive, it is not conclusive. However, if this association is
real, followup of short duration GRBs detected with BATSE or HETE2 should
reveal objects similar to SN1997cy.Comment: 26 pages including 6 postscript figures and 3 tables. Submitted to
ApJ. Re-calibrated photometry - objects are about 0.3mags brighter than in
original versio
Spectroscopic confirmation of an ultra-faint galaxy at the epoch of reionization
Within one billion years of the Big Bang, intergalactic hydrogen was ionized
by sources emitting ultraviolet and higher energy photons. This was the final
phenomenon to globally affect all the baryons (visible matter) in the Universe.
It is referred to as cosmic reionization and is an integral component of
cosmology. It is broadly expected that intrinsically faint galaxies were the
primary ionizing sources due to their abundance in this epoch. However, at the
highest redshifts (; lookback time 13.1 Gyr), all galaxies with
spectroscopic confirmations to date are intrinsically bright and, therefore,
not necessarily representative of the general population. Here, we report the
unequivocal spectroscopic detection of a low luminosity galaxy at . We
detected the Lyman- emission line at {\AA} in two separate
observations with MOSFIRE on the Keck I Telescope and independently with the
Hubble Space Telescope's slit-less grism spectrograph, implying a source
redshift of . The galaxy is gravitationally magnified by
the massive galaxy cluster MACS J1423.8+2404 (), with an estimated
intrinsic luminosity of mag and a stellar mass of
solar masses. Both are an order of
magnitude lower than the four other Lyman- emitters currently known at
, making it probably the most distant representative source of
reionization found to date
Detection of Lyman-Alpha Emission From a Triple Imaged z=6.85 Galaxy Behind MACS J2129.4-0741
We report the detection of Ly emission at \AA{} in the
Keck/DEIMOS and \HST WFC3 G102 grism data from a triply-imaged galaxy at
behind galaxy cluster MACS J2129.40741. Combining the
emission line wavelength with broadband photometry, line ratio upper limits,
and lens modeling, we rule out the scenario that this emission line is \oii at
. After accounting for magnification, we calculate the weighted average
of the intrinsic Ly luminosity to be
and Ly equivalent
width to be \AA{}. Its intrinsic UV absolute magnitude at 1600\AA{} is
mag and stellar mass , making
it one of the faintest (intrinsic ) galaxies with
Ly detection at to date. Its stellar mass is in the typical
range for the galaxies thought to dominate the reionization photon budget at
; the inferred Ly escape fraction is high (\%),
which could be common for sub- galaxies with Ly
emission. This galaxy offers a glimpse of the galaxy population that is thought
to drive reionization, and it shows that gravitational lensing is an important
avenue to probe the sub- galaxy population.Comment: Accepted by ApJ Letter
Spitzer UltRa Faint SUrvey Program (SURFS UP). II. IRAC-Detected Lyman-Break Galaxies at 6 < z < 10 Behind Strong-Lensing Clusters
We study the stellar population properties of the IRAC-detected galaxy candidates from the Spitzer UltRa Faint SUrvey Program
(SURFS UP). Using the Lyman Break selection technique, we find a total of 16
new galaxy candidates at with in at
least one of the IRAC m and m bands. According to the best mass
models available for the surveyed galaxy clusters, these IRAC-detected galaxy
candidates are magnified by factors of --. We find that the
IRAC-detected sample is likely not a homogeneous
galaxy population: some are relatively massive (stellar mass as high as ) and evolved (age Myr) galaxies, while
others are less massive () and very
young ( Myr) galaxies with strong nebular emission lines that boost
their rest-frame optical fluxes. We identify two Ly emitters in our
sample from the Keck DEIMOS spectra, one at (in
RXJ1347) and one at (in MACS0454). We show that IRAC
color, when combined with photometric redshift, can be used to
identify galaxies likely with strong nebular emission lines within certain
redshift windows.Comment: ApJ in pres
RCS2 J232727.6-020437: An Efficient Cosmic Telescope at
We present a detailed gravitational lens model of the galaxy cluster RCS2
J232727.6-020437. Due to cosmological dimming of cluster members and ICL, its
high redshift () makes it ideal for studying background galaxies.
Using new ACS and WFC3/IR HST data, we identify 16 multiple images. From
MOSFIRE follow up, we identify a strong emission line in the spectrum of one
multiple image, likely confirming the redshift of that system to .
With a highly magnified () source plane area of
arcmin at , RCS2 J232727.6-020437 has a lensing efficiency comparable
to the Hubble Frontier Fields clusters. We discover four highly magnified
candidate Lyman-break galaxies behind the cluster, one of which may be
multiply-imaged. Correcting for magnification, we find that all four galaxies
are fainter than . One candidate is detected at in
both Spitzer/IRAC [3.6] and [4.5] channels. A spectroscopic follow-up with
MOSFIRE does not result in the detection of the Lyman-alpha emission line from
any of the four candidates. From the MOSFIRE spectra we place median upper
limits on the Lyman-alpha flux of ().Comment: 14 pages, 9 figures, submitted to ApJ on 3/06/201
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