The current ability of HST to reveal morphological structure in medium-redshift galaxies

Ivan R. King, S. Adam Stanford, Patrick Seitzer, Matthew A. Bershady, William C. Keel, David C. Koo, Nicholas Weir, S. Djorgovski, Rogier Windhorst

Research output: Contribution to journalArticle

11 Citations (Scopus)

Abstract

A pair of FOC f/48 images was taken on a compact galaxy with z∼0.3; and a neighboring field, including a number of medium-redshift galaxies, was covered with the WFC. The conclusions are as follows: (1) The FOC48 (whose field is unlikely to include more than the single galaxy that is targeted) gives a good resolved image of a compact galaxy at blue magnitude J = 20.5 in a single-orbit exposure; longer exposures would (a) add detail to compact galaxies, or (b) allow morphological classification of objects of lower surface brightness. (2) WFC images have a survey capability that can include many galaxies per field, with sufficient resolving power to distinguish clearly between galaxies and stars down to the level of 0.″2 (FWHM), depending on signal-to-noise ratio, and a reasonable capacity for morphology. (3) Although some morphological detail can be discerned in even the aberrated images, deconvolutions very much enhance the ability to see structural detail. Even at the low S/N that is provided by single-orbit exposures the more sophisticated restoration methods offer some advantage over simple Fourier or Lucy techniques. (4) Where image restorations are involved, it is of great importance to have more than one image of each field, so as to compare results and see what is real, and also to facilitate the removal of cosmic rays.

Original languageEnglish (US)
Pages (from-to)1553-1568
Number of pages16
JournalAstronomical Journal
Volume102
Issue number4
StatePublished - Oct 1991

Fingerprint

galaxies
compact galaxies
restoration
orbits
deconvolution
signal-to-noise ratio
cosmic ray
cosmic rays
brightness
signal to noise ratios
stars
exposure

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

King, I. R., Stanford, S. A., Seitzer, P., Bershady, M. A., Keel, W. C., Koo, D. C., ... Windhorst, R. (1991). The current ability of HST to reveal morphological structure in medium-redshift galaxies. Astronomical Journal, 102(4), 1553-1568.

The current ability of HST to reveal morphological structure in medium-redshift galaxies. / King, Ivan R.; Stanford, S. Adam; Seitzer, Patrick; Bershady, Matthew A.; Keel, William C.; Koo, David C.; Weir, Nicholas; Djorgovski, S.; Windhorst, Rogier.

In: Astronomical Journal, Vol. 102, No. 4, 10.1991, p. 1553-1568.

Research output: Contribution to journalArticle

King, IR, Stanford, SA, Seitzer, P, Bershady, MA, Keel, WC, Koo, DC, Weir, N, Djorgovski, S & Windhorst, R 1991, 'The current ability of HST to reveal morphological structure in medium-redshift galaxies', Astronomical Journal, vol. 102, no. 4, pp. 1553-1568.
King IR, Stanford SA, Seitzer P, Bershady MA, Keel WC, Koo DC et al. The current ability of HST to reveal morphological structure in medium-redshift galaxies. Astronomical Journal. 1991 Oct;102(4):1553-1568.
King, Ivan R. ; Stanford, S. Adam ; Seitzer, Patrick ; Bershady, Matthew A. ; Keel, William C. ; Koo, David C. ; Weir, Nicholas ; Djorgovski, S. ; Windhorst, Rogier. / The current ability of HST to reveal morphological structure in medium-redshift galaxies. In: Astronomical Journal. 1991 ; Vol. 102, No. 4. pp. 1553-1568.
@article{139a539e9e414e0385913b8dc6747171,
title = "The current ability of HST to reveal morphological structure in medium-redshift galaxies",
abstract = "A pair of FOC f/48 images was taken on a compact galaxy with z∼0.3; and a neighboring field, including a number of medium-redshift galaxies, was covered with the WFC. The conclusions are as follows: (1) The FOC48 (whose field is unlikely to include more than the single galaxy that is targeted) gives a good resolved image of a compact galaxy at blue magnitude J = 20.5 in a single-orbit exposure; longer exposures would (a) add detail to compact galaxies, or (b) allow morphological classification of objects of lower surface brightness. (2) WFC images have a survey capability that can include many galaxies per field, with sufficient resolving power to distinguish clearly between galaxies and stars down to the level of 0.″2 (FWHM), depending on signal-to-noise ratio, and a reasonable capacity for morphology. (3) Although some morphological detail can be discerned in even the aberrated images, deconvolutions very much enhance the ability to see structural detail. Even at the low S/N that is provided by single-orbit exposures the more sophisticated restoration methods offer some advantage over simple Fourier or Lucy techniques. (4) Where image restorations are involved, it is of great importance to have more than one image of each field, so as to compare results and see what is real, and also to facilitate the removal of cosmic rays.",
author = "King, {Ivan R.} and Stanford, {S. Adam} and Patrick Seitzer and Bershady, {Matthew A.} and Keel, {William C.} and Koo, {David C.} and Nicholas Weir and S. Djorgovski and Rogier Windhorst",
year = "1991",
month = "10",
language = "English (US)",
volume = "102",
pages = "1553--1568",
journal = "Astronomical Journal",
issn = "0004-6256",
publisher = "IOP Publishing Ltd.",
number = "4",

}

TY - JOUR

T1 - The current ability of HST to reveal morphological structure in medium-redshift galaxies

AU - King, Ivan R.

AU - Stanford, S. Adam

AU - Seitzer, Patrick

AU - Bershady, Matthew A.

AU - Keel, William C.

AU - Koo, David C.

AU - Weir, Nicholas

AU - Djorgovski, S.

AU - Windhorst, Rogier

PY - 1991/10

Y1 - 1991/10

N2 - A pair of FOC f/48 images was taken on a compact galaxy with z∼0.3; and a neighboring field, including a number of medium-redshift galaxies, was covered with the WFC. The conclusions are as follows: (1) The FOC48 (whose field is unlikely to include more than the single galaxy that is targeted) gives a good resolved image of a compact galaxy at blue magnitude J = 20.5 in a single-orbit exposure; longer exposures would (a) add detail to compact galaxies, or (b) allow morphological classification of objects of lower surface brightness. (2) WFC images have a survey capability that can include many galaxies per field, with sufficient resolving power to distinguish clearly between galaxies and stars down to the level of 0.″2 (FWHM), depending on signal-to-noise ratio, and a reasonable capacity for morphology. (3) Although some morphological detail can be discerned in even the aberrated images, deconvolutions very much enhance the ability to see structural detail. Even at the low S/N that is provided by single-orbit exposures the more sophisticated restoration methods offer some advantage over simple Fourier or Lucy techniques. (4) Where image restorations are involved, it is of great importance to have more than one image of each field, so as to compare results and see what is real, and also to facilitate the removal of cosmic rays.

AB - A pair of FOC f/48 images was taken on a compact galaxy with z∼0.3; and a neighboring field, including a number of medium-redshift galaxies, was covered with the WFC. The conclusions are as follows: (1) The FOC48 (whose field is unlikely to include more than the single galaxy that is targeted) gives a good resolved image of a compact galaxy at blue magnitude J = 20.5 in a single-orbit exposure; longer exposures would (a) add detail to compact galaxies, or (b) allow morphological classification of objects of lower surface brightness. (2) WFC images have a survey capability that can include many galaxies per field, with sufficient resolving power to distinguish clearly between galaxies and stars down to the level of 0.″2 (FWHM), depending on signal-to-noise ratio, and a reasonable capacity for morphology. (3) Although some morphological detail can be discerned in even the aberrated images, deconvolutions very much enhance the ability to see structural detail. Even at the low S/N that is provided by single-orbit exposures the more sophisticated restoration methods offer some advantage over simple Fourier or Lucy techniques. (4) Where image restorations are involved, it is of great importance to have more than one image of each field, so as to compare results and see what is real, and also to facilitate the removal of cosmic rays.

UR - http://www.scopus.com/inward/record.url?scp=0039306934&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=0039306934&partnerID=8YFLogxK

M3 - Article

AN - SCOPUS:0039306934

VL - 102

SP - 1553

EP - 1568

JO - Astronomical Journal

JF - Astronomical Journal

SN - 0004-6256

IS - 4

ER -