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Papers by Andrew Dolphin
Publications of the Astronomical Society of the Pacific, 2000
Astronomy and Astrophysics
... Affiliation: AA(Max-Planck-Institut für Astronomie, Heidelberg, Germany), AB(National Optical... more ... Affiliation: AA(Max-Planck-Institut für Astronomie, Heidelberg, Germany), AB(National Optical Astronomy Observatoires, Tucson, USA), AC(UCO/Lick Observatory, UCSC, Santa Cruz, USA). ...And I is the least luminous galaxy in which a globular cluster has been detected so far. ...
Young star clusters provide a unique indicator as to the past star formation of a galaxy. In addi... more Young star clusters provide a unique indicator as to the past star formation of a galaxy. In addition to providing a fossil record of past star formation activity {similarly to the stellar content}, it appears that the amount and nature of cluster formation depends strongly on the environmental conditions. The nature of these objects {indistinguishable from bright or foreground stars from the ground} has made a detailed study difficult in the past; the advent of textitHST and its superior resolution circumvents this problem. Previous textitHST studies have focused on interacting systems and merger remnants {where young clusters are expected to be abundant}, leaving a number of questions unanswered, such as: {1} Is the ratio of massive cluster formation to total star formation constant? {2} Are trends {if any} along the Hubble sequence analogous to those seen in larger OB associations and HII regions? We propose to address these and other questions through a survey of t. he. cluster ...
The Astrophysical Journal, 2014
ABSTRACT We measured the Tip of the Red Giant Branch distances to nine galaxies in the direction ... more ABSTRACT We measured the Tip of the Red Giant Branch distances to nine galaxies in the direction to the Virgo cluster using the Advanced Camera for Surveys on the Hubble Space Telescope. These distances put seven galaxies: GR 34, UGC 7512, NGC 4517, IC 3583, NGC 4600, VCC 2037 and KDG 215 in front of the Virgo, and two galaxies: IC 3023, KDG 177 likely inside the cluster. Distances and radial velocities of the galaxies situated between us and the Virgo core clearly exhibit the infall phenomenon toward the cluster. In the case of spherically symmetric radial infall we estimate the radius of the "zero-velocity surface" to be (7.2+-0.7) Mpc that yields the total mass of the Virgo cluster to be (8.0+-2.3) X 10^{14} M_sun in good agreement with its virial mass estimates. We conclude that the Virgo outskirts does not contain significant amounts of dark matter beyond its virial radius.
The Astronomical Journal, 2002
ABSTRACT
Publications of the Astronomical Society of the Pacific, 2009
... Andrew E. Dolphin ... An initial solution to this was to cool the camera from −76◦C to −88◦C ... more ... Andrew E. Dolphin ... An initial solution to this was to cool the camera from −76◦C to −88◦C to reduce the magnitude of the effect, and to apply a correction that scaled from linearly from zero for starswith Y = 0 to a maximum of 0.04 magnitudes for stars with Y = 800. Holtzman et al. ...
Publications of the Astronomical Society of the Pacific, 2000
ABSTRACT
Monthly Notices of the Royal Astronomical Society, 2002
Publications of the Astronomical Society of the Pacific, 2000
Astronomy and Astrophysics
... Affiliation: AA(Max-Planck-Institut für Astronomie, Heidelberg, Germany), AB(National Optical... more ... Affiliation: AA(Max-Planck-Institut für Astronomie, Heidelberg, Germany), AB(National Optical Astronomy Observatoires, Tucson, USA), AC(UCO/Lick Observatory, UCSC, Santa Cruz, USA). ...And I is the least luminous galaxy in which a globular cluster has been detected so far. ...
Young star clusters provide a unique indicator as to the past star formation of a galaxy. In addi... more Young star clusters provide a unique indicator as to the past star formation of a galaxy. In addition to providing a fossil record of past star formation activity {similarly to the stellar content}, it appears that the amount and nature of cluster formation depends strongly on the environmental conditions. The nature of these objects {indistinguishable from bright or foreground stars from the ground} has made a detailed study difficult in the past; the advent of textitHST and its superior resolution circumvents this problem. Previous textitHST studies have focused on interacting systems and merger remnants {where young clusters are expected to be abundant}, leaving a number of questions unanswered, such as: {1} Is the ratio of massive cluster formation to total star formation constant? {2} Are trends {if any} along the Hubble sequence analogous to those seen in larger OB associations and HII regions? We propose to address these and other questions through a survey of t. he. cluster ...
The Astrophysical Journal, 2014
ABSTRACT We measured the Tip of the Red Giant Branch distances to nine galaxies in the direction ... more ABSTRACT We measured the Tip of the Red Giant Branch distances to nine galaxies in the direction to the Virgo cluster using the Advanced Camera for Surveys on the Hubble Space Telescope. These distances put seven galaxies: GR 34, UGC 7512, NGC 4517, IC 3583, NGC 4600, VCC 2037 and KDG 215 in front of the Virgo, and two galaxies: IC 3023, KDG 177 likely inside the cluster. Distances and radial velocities of the galaxies situated between us and the Virgo core clearly exhibit the infall phenomenon toward the cluster. In the case of spherically symmetric radial infall we estimate the radius of the "zero-velocity surface" to be (7.2+-0.7) Mpc that yields the total mass of the Virgo cluster to be (8.0+-2.3) X 10^{14} M_sun in good agreement with its virial mass estimates. We conclude that the Virgo outskirts does not contain significant amounts of dark matter beyond its virial radius.
The Astronomical Journal, 2002
ABSTRACT
Publications of the Astronomical Society of the Pacific, 2009
... Andrew E. Dolphin ... An initial solution to this was to cool the camera from −76◦C to −88◦C ... more ... Andrew E. Dolphin ... An initial solution to this was to cool the camera from −76◦C to −88◦C to reduce the magnitude of the effect, and to apply a correction that scaled from linearly from zero for starswith Y = 0 to a maximum of 0.04 magnitudes for stars with Y = 800. Holtzman et al. ...
Publications of the Astronomical Society of the Pacific, 2000
ABSTRACT
Monthly Notices of the Royal Astronomical Society, 2002