[ITAL]Hubble Space Telescope[/ITAL] Space Telescope Imaging Spectrograph Imaging of the Host Galaxy of GRB 980425/SN 1998[CLC]bw[/CLC]

Secure measurements of the mass of the central supermassive black hole, MBH, in external galaxies are traditionally obtained through the modeling of the stellar and/or gaseous kinematics, most often derived using Hubble Space Telescope (HST) observations in the optical domain. The modeling of the nuclear ionized-gas kinematics has led to accurate MBH measurements at a relatively cheap cost in terms of observation time compared to stellar-dynamical MBH determinations. But only a handful of the objects have turned out to have sufficiently regular gas velocity fields for the purpose of modeling. Nevertheless, the HST archive contains a yet untapped resource that can be used to better constrain the MBH budget across the different morphological types of galaxies, which consists of the vast number of the Space Telescope Imaging Spectrograph (STIS) spectra from which a central emission-line width can be measured. These data allow to put an upper limit on MBH for a large number of galaxies and promise to compensate for the lack of exact measurements when studying the MBH–host galaxy relationships.

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Quasar host galaxy images from the Hubble Space Telescope Archive

Monthly Notices of the Royal Astronomical Society ◽

10.1046/j.1365-8711.1999.02281.x ◽

1999 ◽

Vol 302 (2) ◽

pp. L39-L44 ◽

Cited By ~ 26

Author(s):

P. J. Boyce ◽

M. J. Disney ◽

D. G. Bleaken

Keyword(s):

Hubble Space Telescope ◽

Host Galaxy ◽

Space Telescope

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Inspecting the Cepheid Distance Ladder: the Hubble Space Telescope Distance to the SN Ia Host Galaxy NGC 5584

The Astrophysical Journal ◽

10.3847/1538-4357/abe7e5 ◽

2021 ◽

Vol 911 (1) ◽

pp. 12

Author(s):

Behnam Javanmardi ◽

Antoine Mérand ◽

Pierre Kervella ◽

Louise Breuval ◽

Alexandre Gallenne ◽

...

Keyword(s):

Hubble Space Telescope ◽

Host Galaxy ◽

Space Telescope

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Very Large Telescope and [ITAL]Hubble Space Telescope[/ITAL] Observations of the Host Galaxy of GRB 990705

The Astrophysical Journal ◽

10.1086/346072 ◽

2002 ◽

Vol 581 (2) ◽

pp. L81-L84 ◽

Cited By ~ 41

Author(s):

E. Le Floc’h ◽

P.-A. Duc ◽

I. F. Mirabel ◽

D. B. Sanders ◽

G. Bosch ◽

...

Keyword(s):

Hubble Space Telescope ◽

Host Galaxy ◽

Large Telescope ◽

Space Telescope ◽

Very Large Telescope

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The Interstellar Abundance of Lead: Experimental Oscillator Strengths for Pb ii λ1203 and λ1433 and New Detections of Pb ii in the Interstellar Medium

Proceedings of the International Astronomical Union ◽

10.1017/s1743921317005038 ◽

2015 ◽

Vol 11 (A29A) ◽

Author(s):

A. M. Ritchey ◽

N. Heidarian ◽

R. E. Irving ◽

S. R. Federman ◽

D. G. Ellis ◽

...

Keyword(s):

Interstellar Medium ◽

Hubble Space Telescope ◽

Oscillator Strengths ◽

Interstellar Gas ◽

Lifetime Measurements ◽

Space Telescope ◽

Interstellar Grains ◽

Imaging Spectrograph ◽

Theoretical Results ◽

Beam Foil

AbstractWe present the first experimentally determined oscillator strengths for the Pb ii transitions at 1203.6 Å and 1433.9 Å, obtained from lifetime measurements made using beam-foil techniques. We also present new detections of these lines in the interstellar medium from an analysis of archival spectra acquired by the Space Telescope Imaging Spectrograph onboard the Hubble Space Telescope. Our observations of the Pb ii λ1203 line represent the first detection of this transition in interstellar gas. Our experimental f-values for the Pb ii λ1203 and λ1433 transitions are consistent with recent theoretical results, including our own relativistic calculations, but are significantly smaller than previous values based on older calculations. Our new f-value for Pb ii λ1433 (0.321 ± 0.034) yields an increase in the interstellar abundance of Pb of 0.43 dex over estimates based on the f-value listed by Morton. With our revised f-values, and with our new detections of Pb ii λ1203 and λ1433, we find that the depletion of Pb onto interstellar grains is not nearly as severe as previously thought, and is very similar to the depletions seen for elements such as Zn and Sn, which have similar condensation temperatures.

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The Space Telescope Imaging Spectrograph

Highlights of Astronomy ◽

10.1017/s1539299600008145 ◽

1989 ◽

Vol 8 ◽

pp. 445-448

Author(s):

Bruce E Woodgate

Keyword(s):

First Generation ◽

Second Generation ◽

Hubble Space Telescope ◽

Space Telescope ◽

Infra Red ◽

Imaging Spectrograph

The Space Telescope Imaging Spectrograph (STIS) is a second generation instrument to be installed into the Hubble Space Telescope (HST) in-orbit 5–9 years after the first launch. Together with the infra-red instrument, it will provide a large increase in capability of the observatory, and be able to replace a first generation that had failed or degraded.

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

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1039 ◽

2019 ◽

Vol 486 (3) ◽

pp. 3105-3117 ◽

Cited By ~ 1

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.

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