Imaging of [CLC][ITAL]z[/ITAL][/CLC] ∼ 2 QSO Host Galaxies with the [ITAL]Hubble Space Telescope[/ITAL]

2002 ◽  
Vol 123 (6) ◽  
pp. 2936-2944 ◽  
Author(s):  
J. B. Hutchings ◽  
D. Frenette ◽  
R. Hanisch ◽  
J. Mo ◽  
P. J. Dumont ◽  
...  
Keyword(s):  
Hubble Space Telescope ◽  
Host Galaxies ◽  
Space Telescope

scholarly journals Chandra and Hubble Space Telescope observations of dark gamma-ray bursts and their host galaxies

2019 ◽  
Vol 486 (3) ◽  
pp. 3105-3117 ◽  
Author(s):  
A A Chrimes ◽  
A J Levan ◽  
E R Stanway ◽  
J D Lyman ◽  
A S Fruchter ◽  
...  
Keyword(s):  
Morphological Analysis ◽  
Gamma Ray ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Host Population ◽  
Host Galaxy ◽  
Host Galaxies ◽  
Space Telescope ◽  
X Ray ◽  
Dust Component

Abstract We present a study of 21 dark gamma-ray burst (GRB) host galaxies, predominantly using X-ray afterglows obtained with the Chandra X-Ray Observatory (CXO) to precisely locate the burst in deep Hubble Space Telescope (HST) imaging of the burst region. The host galaxies are well-detected in F160W in all but one case and in F606W imaging in 60 per cent of cases. We measure magnitudes and perform a morphological analysis of each galaxy. The asymmetry, concentration, and ellipticity of the dark burst hosts are compared against the host galaxies of optically bright GRBs. In agreement with other studies, we find that dark GRB hosts are redder and more luminous than the bulk of the GRB host population. The distribution of projected spatial offsets for dark GRBs from their host galaxy centroids is comparable to that of optically bright bursts. The dark GRB hosts are physically larger, more massive and redder, but are morphologically similar to the hosts of bright GRBs in terms of concentration and asymmetry. Our analysis constrains the fraction of high redshift (z > 5) GRBs in the sample to 14 per cent, implying an upper limit for the whole long-GRB population of ≤4.4 per cent. If dust is the primary cause of afterglow darkening amongst dark GRBs, the measured extinction may require a clumpy dust component in order to explain the observed offset and ellipticity distributions.

scholarly journals Galaxies with Binary Nuclei

2013 ◽  
Vol 9 (S304) ◽  
pp. 363-370
Author(s):  
Yervant Terzian ◽  
Edward Khachikian
Keyword(s):  
Hubble Space Telescope ◽  
Radio Galaxies ◽  
Active Galaxies ◽  
Emission Lines ◽  
Special Astrophysical Observatory ◽  
Host Galaxies ◽  
Strong Emission ◽  
Space Telescope ◽  
Byurakan Astrophysical Observatory ◽  
The Common

AbstractIt is known that among active galaxies (AG) with strong emission lines (UV-galaxies, Sy1 and Sy2, Markarian and Kazarian galaxies, radio-galaxies, QSOs host galaxies and so on) there is a large percentage of objects with double and multiple (or complex) nuclei. The common sizes of these nuclei are of the order of a few hundred parsecs or kiloparsecs. We shall discuss the results of morphological and spectroscopic observations of a number of “active galaxies” carried out with the 5m Palomar telescope, 2.6m telescope of Ambartsumian Byurakan Astrophysical Observatory, 6m telescope of Special Astrophysical Observatory in Russia, and newer Hubble Space Telescope data.

scholarly journals The Hubble Space Telescope Key Project to Measure the Hubble Constant

1999 ◽  
Vol 183 ◽  
pp. 17-30 ◽  
Author(s):  
Wendy L. Freedman ◽  
Jeremy R. Mould ◽  
Robert C. Kennicutt ◽  
Barry F. Madore
Keyword(s):  
Hubble Space Telescope ◽  
Hubble Constant ◽  
Distance Scale ◽  
General Assembly ◽  
Host Galaxies ◽  
Space Telescope ◽  
Type Ia Supernova ◽  
Type Ia ◽  
Extragalactic Distance Scale

A Joint Discussion on the extragalactic distance scale and the Hubble constant took place fifteen years ago, at the 1982 XVIIIth General Assembly of the IAU, held in Patras, Greece. At that time, the newest applications of infrared photometers to Tully-Fisher measurements (Aaronson 1983) and Cepheid distances (Madore 1983) were reported. CCDs were just coming into use and had not yet been applied to extragalactic distance determinations; all of the extragalactic Cepheid distances were based on photographic Argelander (eye-estimated) photometry (Tammann and Sandage 1983 and references therein). No Cepheid distances to type Ia supernova-host galaxies were available.

scholarly journals Massive stars in extremely metal-poor galaxies: a window into the past

2021 ◽  
Author(s):  
Miriam Garcia ◽  
Christopher J. Evans ◽  
Joachim M. Bestenlehner ◽  
Jean Claude Bouret ◽  
Norberto Castro ◽  
...  
Keyword(s):  
Metal Content ◽  
Hubble Space Telescope ◽  
Massive Stars ◽  
Current Knowledge ◽  
Single Point ◽  
White Paper ◽  
Host Galaxies ◽  
New Paradigm ◽  
Space Telescope ◽  
The Universe

AbstractCosmic history has witnessed the lives and deaths of multiple generations of massive stars, all of them invigorating their host galaxies with ionizing photons, kinetic energy, fresh material, and stellar-mass black holes. Ubiquitous engines as they are, astrophysics needs a good understanding of their formation, evolution, properties and yields throughout the history of the Universe, and with decreasing metal content mimicking the environment at the earliest epochs. Ultimately, a physical model that could be extrapolated to zero metallicity would enable tackling long-standing questions such as “What did the first, very massive stars of the Universe look like?” or “What was their role in the re-ionization of the Universe?” Yet, most of our knowledge of metal-poor massive stars is drawn from one single point in metallicity. Massive stars in the Small Magellanic Cloud (SMC, $\sim $ ∼ 1/5Z⊙ ) currently serve as templates for low-metallicity objects in the early Universe, even though significant differences with respect to massive stars with poorer metal content have been reported. This White Paper summarizes the current knowledge on extremely (sub-SMC) metal poor massive stars, highlighting the most outstanding open questions and the need to supersede the SMC as standard. A new paradigm can be built from nearby extremely metal-poor galaxies that make a new metallicity ladder, but massive stars in these galaxies are out of reach to current observational facilities. Such a task would require an L-size mission, consisting of a 10m-class space telescope operating in the optical and the ultraviolet ranges. Alternatively, we propose that ESA unites efforts with NASA to make the LUVOIR mission concept a reality, thus continuing the successful partnership that made the Hubble Space Telescope one of the greatest observatories of all time.

scholarly journals Hunting for the faintest hosts of the brightest supernovae

2015 ◽  
Vol 11 (A29B) ◽  
pp. 259-260
Author(s):  
Charlotte R. Angus ◽  
Andrew J. Levan ◽  
Daniel A. Perley
Keyword(s):  
Near Infrared ◽  
Hubble Space Telescope ◽  
Light Curves ◽  
Core Collapse ◽  
Host Galaxies ◽  
Space Telescope ◽  
Order Of Magnitude

AbstractSuperluminous supernovae (SLSNe) are an emerging class of SNe that exhibit luminosities exceeding those of SN Ia by an order of magnitude and have light curves with characteristic timescales of hundreds of days. Here we present observations of the host galaxies of 21 SLSNe observed with the Hubble Space Telescope, and show that their ultraviolet (UV) and near-infrared (nIR) luminosities and sizes and very different from those of the hosts of other core collapse events, with significant implications for their progenitors.

scholarly journals HUBBLE SPACE TELESCOPE Imaging of the Host Galaxies of High‐Redshift Radio‐loud Quasars

1999 ◽  
Vol 124 (1) ◽  
pp. 11-31 ◽  
Author(s):  
Matthew D. Lehnert ◽  
Wil J. M. van Breugel ◽  
Timothy M. Heckman ◽  
George K. Miley
Keyword(s):  
Hubble Space Telescope ◽  
High Redshift ◽  
Host Galaxies ◽  
Space Telescope
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