We present optical spectroscopy of the host galaxies of 4 QSO's: PG1444+407, PKS 2349-147, 3C 323... more We present optical spectroscopy of the host galaxies of 4 QSO's: PG1444+407, PKS 2349-147, 3C 323.1, and 4C 31.63 having a redshift range (0.1 < z < 0.3). The spectra were obtained at the Keck Observatory with the LRIS instrument offset 2-4 arcseconds from the nucleus at several position angles in each galaxy. The objects close to 3C 323.1 and PKS 2349-147 have the same redshifts of their nearby QSOs and appear to be the nuclei of galaxies in the final states of merging with the host galaxies. The spectra of the hosts show some variety: PKS 2349-147 and 3C 323.1 show strong off-nuclear emission lines plus stellar absorption features, while the other two show only stellar absorption. PKS 2349-147 and PG 1444+407 have a mixture of old and moderately young stars, while 4C 31.63 has the spectrum of a normal giant elliptical, which is very rare in our larger sample. The spectrum of the host of 3C 323.1 appears to dominated by older stars, though our data for it are of lower quality. The redshifts of the off-nucleus emission lines and stellar components are very close to those of the associated QSOs.
We present optical spectroscopy of the host galaxies of four quasi-stellar objects (QSOs)-PG 1444... more We present optical spectroscopy of the host galaxies of four quasi-stellar objects (QSOs)-PG 1444+407, PKS 2349-147, 3C 323.1, and 4C 31.63-having a redshift range 0.1<=z<=0.3. The spectra were obtained at the Keck Observatory with the Low Resolution Imaging Spectrograph instrument offset 2"-4" from the nucleus at several position angles in each galaxy. The objects close to 3C 323.1 and PKS 2349-147 have the same redshifts as their nearby QSOs and appear to be the nuclei of galaxies in the final states of merging with the host galaxies. The spectra of the hosts show some variety: PKS 2349-147 and 3C 323.1 show strong off-nuclear emission lines plus stellar absorption features, while the other two show only stellar absorption. PKS 2349-147 and PG 1444+407 have a mixture of old and moderately young stars, while 4C 31.63 has the spectrum of a normal giant elliptical galaxy, which is very rare in our larger sample. The spectrum of the host of 3C 323.1 appears to be dominated by older stars, although our data for it are of lower quality. The redshifts of the off-nucleus emission lines and stellar components are very close to those of the associated QSOs.
A strong connection between AGN and galaxy evolution has emerged over the past decade. One way to... more A strong connection between AGN and galaxy evolution has emerged over the past decade. One way to investigate how this connection arises is to study the properties of the host galaxies of quasars, in which the galaxy is actively feeding the supermassive black hole (BH) and both BH and galaxy should be growing. We present stellar velocity dispersion, σ*, measurements in the host galaxies of 8 luminous quasars (MV < -23) using the Ca H&K lines in off-nuclear spectra. We combine these data with effective radii, Re, and surface brightnesses, μe, to place the hosts on the Fundamental Plane (FP) where their properties are compared to other types of galaxies. We find that the radio-loud (RL) QSO hosts have similar properties to massive early-type galaxies, while the radio-quiet (RQ) hosts are more similar to intermediate-mass early-types. The RL hosts lie at the upper extreme of the FP due to their higher σ* ( 351 km s-1), lower μe(r) ( 20.8 mag arcsec-2), and larger Re ( 11.6 kpc); and they have <M*> = 1.9 x 1012 Msun and <M/L> = 14.1. In contrast, properties of the RQ hosts are σ* 198 km s-1, μe(r) 19.5 mag arcsec-2, Re 5.4 kpc, M* 3.5 x 1011 Msun, and M/L 3.5. The distinction between these galaxies appears to be mass, with the separation occurring at σ* 300 km s-1 and M* 7 x 1011 Msun. Our data support previous results that PG QSOs are related to gas-rich galaxy mergers that form intermediate-mass galaxies, while RL QSOs reside in massive early-type galaxies, some of which show signs of recent mergers. Most previous work has drawn these conclusions by inferring host galaxy properties from estimated BH mass, while here we have relied purely on directly measured host galaxy properties.
... Page 8. 44 OPTICS IN ASTROPHYSICS Figure 3. The first 12 Zernike polynomials (see text) eye. ... more ... Page 8. 44 OPTICS IN ASTROPHYSICS Figure 3. The first 12 Zernike polynomials (see text) eye. The principle is the same, a Newtonian telescope is really just a parabolic mirror. 6. Two Mirror telescopes ... ASA = 1 128F3 1 { K1 + 1 − 1+∆ m + 1 ( m − 1 m + 1 )3 [ K2 + ( m + 1 m − 1 ...
The Echellette Spectrograph and Imager (ESI), currently being developed for use at the Cassegrain... more The Echellette Spectrograph and Imager (ESI), currently being developed for use at the Cassegrain focus of the Keck II 10-m telescope, employs two large (25 kg) prisms for cross dispersion. In order to maintain optical stability in the spectroscopic modes, these prisms must maintain a fixed angle relative to the nominal spectrograph optical axis under a variety of flexural and
While recent work with HST has provided strong evidence that most relatively nearby QSOs are imbe... more While recent work with HST has provided strong evidence that most relatively nearby QSOs are imbedded in nebulosity, identification of the nature of the nebulosity requires spectroscopic observations. We present spectra of the off-nuclear light of eight QSOs obtained with the LRIS spectrograph of the Keck Telescope. The majority of these clearly show the absorption spectra of the stars of a host galaxy at the same redshift as the QSO. In addition, emission lines from gas are evident in the nebulosities, and for one object, PG 0052+251, we detect the spectra of several H II regions along a spiral arm. The QSO PKS 2349-014 is particularly interesting, as spectra taken at several positions show that the surrounding nebulosity, the apparently tidal wisps, and the companion close to the QSO all have stellar absorpton lines at the same redshift as the QSO. These data show that if one wishes to ascribe non-cosmological redshifts to these QSOs, the entire surrounding galaxies and nearby companions must also have non-cosmological redshifts. The data add additional support for the evolutionary scheme for QSOs and AGN published previously (J. Miller, Proc.N.A.S., Vol. 92, 11422, 1995).
Adaptive Optics For Large Telescopes Topical Meeting, 1992
The survey studies the local boundary layer effects over an 18-acre geographic area atop Mt. Hale... more The survey studies the local boundary layer effects over an 18-acre geographic area atop Mt. Haleakala, a 10,000-ft. dormant volcano located in Maui, Hawaii, and therefrom to determine the best location for a new 4 m class telescope proposed for Haleakala.
We present optical ( 4000Å - 8000Å) off-nuclear spectroscopy of the host galaxies of 4 QSO's, PG1... more We present optical ( 4000Å - 8000Å) off-nuclear spectroscopy of the host galaxies of 4 QSO's, PG1444+407, PKS2349-147, 3c323.1, and 4c31.63, with red-shift range ( 0.1 < z < 0.3). The spectra were taken from 2-4 arcseconds from the nucleus at several position angles around each galaxy. They were obtained at Keck Observatory with the Low Resolution Imaging Spectrograph (LRIS) and the Echellette Spectrograph and Imager (ESI) between 1996 and 2001. Some of the spectra show stellar absorption features indicative of the underlying old stellar populations of the host galaxies mixed with other components such as high-ionization emission-line gas and in some cases, a young stellar component. Some of the spectra show an intriguing featureless continuum. The redshifts of the off-nuclear emission lines and stellar components are very close to those of the QSOs. In addition, we compare these spectra to Bruzual and Charlot population synthesis models.
NATO Science Series II: Mathematics, Physics and Chemistry, 2006
We present the basics of optical design as it applies to two mirrored telescope systems. We discu... more We present the basics of optical design as it applies to two mirrored telescope systems. We discuss Zernike decomposition of wave-front error and the description of Strehl in terms of small Zernike errors. We also discuss the balancing of aberrations for a two mirror system and present the Ritchey-Chrétien design as an example of a zero coma system.
Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, 2003
We present the design and status report on the development of an Integral Field Unit (IFU) for th... more We present the design and status report on the development of an Integral Field Unit (IFU) for the Echellette spectrograph and imager (ESI), a recently developed R=13000, Cassegrain spectrograph at Keck II. We have designed a family of IFU&amp;quot;s for the spectrograph, providing a range of field-coverages and dispersions. The optical designs are based on the Advanced Image Slicer concept
We present optical spectroscopy of the host galaxies of 4 QSO's: PG 1444+407, PKS 2349-147, 3C 32... more We present optical spectroscopy of the host galaxies of 4 QSO's: PG 1444+407, PKS 2349-147, 3C 323.1, and 4C 31.63 having a redshift range 0.1 ≤ z ≤ 0.3. The spectra were obtained at the Keck Observatory with the LRIS instrument offset 2-4 arcseconds from the nucleus at several position angles in each galaxy. The objects close to 3C 323.1 and PKS 2349-147 have the same redshifts of their nearby QSOs and appear to be the nuclei of galaxies in the final states of merging with the host galaxies. The spectra of the hosts show some variety: PKS 2349-147 and 3C 323.1 show strong off-nuclear emission lines plus stellar absorption features, while the other two show only stellar absorption. PKS 2349-147 and PG 1444+407 have a mixture of old and moderately young stars, while 4C 31.63 has the spectrum of a normal giant elliptical, which is very rare in our larger sample. The spectrum of the host of 3C 323.1 appears to dominated by older stars, though our data for it are of lower quality. The redshifts of the off-nucleus emission lines and stellar components are very close to those of the associated QSOs.
We present stellar velocity dispersion measurements in the host galaxies of 10 luminous quasars (... more We present stellar velocity dispersion measurements in the host galaxies of 10 luminous quasars (M V < −23) using the Ca H&K lines in off-nuclear spectra. We combine these data with effective radii and magnitudes from the literature to place the host galaxies on the Fundamental Plane (FP) where their properties are compared to other types of galaxies. We find that the radio-loud (RL) QSO hosts have similar properties to massive elliptical galaxies, while the radio-quiet (RQ) hosts are more similar to intermediate mass galaxies. The RL hosts lie at the upper extreme of the FP due to their large velocity dispersions ( σ * = 321 km s −1 ), low surface brightness ( µ e (r) = 20.8 mag arcsec −2 ), and large effective radii ( R e = 11.4 kpc), and have M * = 1.5 x 10 12 M ⊙ and M/L = 12.4. In contrast, properties of the RQ hosts are σ * = 241 km s −1 , M * ∼ 4.4 x 10 11 M ⊙ , and M/L ∼ 5.3. The distinction between these galaxies occurs at σ * ∼ 300 km s −1 , R e ∼ 6 kpc, and corresponding M * ∼ 5.9 ± 3.5 x 10 11 M ⊙ . Our data support previous results that PG QSOs are related to gas-rich galaxy mergers that form intermediate-mass galaxies, while RL QSOs reside in massive early-type galaxies, most of which also show signs of recent mergers or interactions. Most previous work has drawn these conclusions by using estimates of the black hole mass and inferring host galaxy properties from that, while here we have relied purely on directly measured host galaxy properties.
We present optical spectroscopy of the host galaxies of 4 QSO's: PG1444+407, PKS 2349-147, 3C 323... more We present optical spectroscopy of the host galaxies of 4 QSO's: PG1444+407, PKS 2349-147, 3C 323.1, and 4C 31.63 having a redshift range (0.1 < z < 0.3). The spectra were obtained at the Keck Observatory with the LRIS instrument offset 2-4 arcseconds from the nucleus at several position angles in each galaxy. The objects close to 3C 323.1 and PKS 2349-147 have the same redshifts of their nearby QSOs and appear to be the nuclei of galaxies in the final states of merging with the host galaxies. The spectra of the hosts show some variety: PKS 2349-147 and 3C 323.1 show strong off-nuclear emission lines plus stellar absorption features, while the other two show only stellar absorption. PKS 2349-147 and PG 1444+407 have a mixture of old and moderately young stars, while 4C 31.63 has the spectrum of a normal giant elliptical, which is very rare in our larger sample. The spectrum of the host of 3C 323.1 appears to dominated by older stars, though our data for it are of lower quality. The redshifts of the off-nucleus emission lines and stellar components are very close to those of the associated QSOs.
We present optical spectroscopy of the host galaxies of four quasi-stellar objects (QSOs)-PG 1444... more We present optical spectroscopy of the host galaxies of four quasi-stellar objects (QSOs)-PG 1444+407, PKS 2349-147, 3C 323.1, and 4C 31.63-having a redshift range 0.1<=z<=0.3. The spectra were obtained at the Keck Observatory with the Low Resolution Imaging Spectrograph instrument offset 2"-4" from the nucleus at several position angles in each galaxy. The objects close to 3C 323.1 and PKS 2349-147 have the same redshifts as their nearby QSOs and appear to be the nuclei of galaxies in the final states of merging with the host galaxies. The spectra of the hosts show some variety: PKS 2349-147 and 3C 323.1 show strong off-nuclear emission lines plus stellar absorption features, while the other two show only stellar absorption. PKS 2349-147 and PG 1444+407 have a mixture of old and moderately young stars, while 4C 31.63 has the spectrum of a normal giant elliptical galaxy, which is very rare in our larger sample. The spectrum of the host of 3C 323.1 appears to be dominated by older stars, although our data for it are of lower quality. The redshifts of the off-nucleus emission lines and stellar components are very close to those of the associated QSOs.
A strong connection between AGN and galaxy evolution has emerged over the past decade. One way to... more A strong connection between AGN and galaxy evolution has emerged over the past decade. One way to investigate how this connection arises is to study the properties of the host galaxies of quasars, in which the galaxy is actively feeding the supermassive black hole (BH) and both BH and galaxy should be growing. We present stellar velocity dispersion, σ*, measurements in the host galaxies of 8 luminous quasars (MV < -23) using the Ca H&K lines in off-nuclear spectra. We combine these data with effective radii, Re, and surface brightnesses, μe, to place the hosts on the Fundamental Plane (FP) where their properties are compared to other types of galaxies. We find that the radio-loud (RL) QSO hosts have similar properties to massive early-type galaxies, while the radio-quiet (RQ) hosts are more similar to intermediate-mass early-types. The RL hosts lie at the upper extreme of the FP due to their higher σ* ( 351 km s-1), lower μe(r) ( 20.8 mag arcsec-2), and larger Re ( 11.6 kpc); and they have <M*> = 1.9 x 1012 Msun and <M/L> = 14.1. In contrast, properties of the RQ hosts are σ* 198 km s-1, μe(r) 19.5 mag arcsec-2, Re 5.4 kpc, M* 3.5 x 1011 Msun, and M/L 3.5. The distinction between these galaxies appears to be mass, with the separation occurring at σ* 300 km s-1 and M* 7 x 1011 Msun. Our data support previous results that PG QSOs are related to gas-rich galaxy mergers that form intermediate-mass galaxies, while RL QSOs reside in massive early-type galaxies, some of which show signs of recent mergers. Most previous work has drawn these conclusions by inferring host galaxy properties from estimated BH mass, while here we have relied purely on directly measured host galaxy properties.
... Page 8. 44 OPTICS IN ASTROPHYSICS Figure 3. The first 12 Zernike polynomials (see text) eye. ... more ... Page 8. 44 OPTICS IN ASTROPHYSICS Figure 3. The first 12 Zernike polynomials (see text) eye. The principle is the same, a Newtonian telescope is really just a parabolic mirror. 6. Two Mirror telescopes ... ASA = 1 128F3 1 { K1 + 1 − 1+∆ m + 1 ( m − 1 m + 1 )3 [ K2 + ( m + 1 m − 1 ...
The Echellette Spectrograph and Imager (ESI), currently being developed for use at the Cassegrain... more The Echellette Spectrograph and Imager (ESI), currently being developed for use at the Cassegrain focus of the Keck II 10-m telescope, employs two large (25 kg) prisms for cross dispersion. In order to maintain optical stability in the spectroscopic modes, these prisms must maintain a fixed angle relative to the nominal spectrograph optical axis under a variety of flexural and
While recent work with HST has provided strong evidence that most relatively nearby QSOs are imbe... more While recent work with HST has provided strong evidence that most relatively nearby QSOs are imbedded in nebulosity, identification of the nature of the nebulosity requires spectroscopic observations. We present spectra of the off-nuclear light of eight QSOs obtained with the LRIS spectrograph of the Keck Telescope. The majority of these clearly show the absorption spectra of the stars of a host galaxy at the same redshift as the QSO. In addition, emission lines from gas are evident in the nebulosities, and for one object, PG 0052+251, we detect the spectra of several H II regions along a spiral arm. The QSO PKS 2349-014 is particularly interesting, as spectra taken at several positions show that the surrounding nebulosity, the apparently tidal wisps, and the companion close to the QSO all have stellar absorpton lines at the same redshift as the QSO. These data show that if one wishes to ascribe non-cosmological redshifts to these QSOs, the entire surrounding galaxies and nearby companions must also have non-cosmological redshifts. The data add additional support for the evolutionary scheme for QSOs and AGN published previously (J. Miller, Proc.N.A.S., Vol. 92, 11422, 1995).
Adaptive Optics For Large Telescopes Topical Meeting, 1992
The survey studies the local boundary layer effects over an 18-acre geographic area atop Mt. Hale... more The survey studies the local boundary layer effects over an 18-acre geographic area atop Mt. Haleakala, a 10,000-ft. dormant volcano located in Maui, Hawaii, and therefrom to determine the best location for a new 4 m class telescope proposed for Haleakala.
We present optical ( 4000Å - 8000Å) off-nuclear spectroscopy of the host galaxies of 4 QSO's, PG1... more We present optical ( 4000Å - 8000Å) off-nuclear spectroscopy of the host galaxies of 4 QSO's, PG1444+407, PKS2349-147, 3c323.1, and 4c31.63, with red-shift range ( 0.1 < z < 0.3). The spectra were taken from 2-4 arcseconds from the nucleus at several position angles around each galaxy. They were obtained at Keck Observatory with the Low Resolution Imaging Spectrograph (LRIS) and the Echellette Spectrograph and Imager (ESI) between 1996 and 2001. Some of the spectra show stellar absorption features indicative of the underlying old stellar populations of the host galaxies mixed with other components such as high-ionization emission-line gas and in some cases, a young stellar component. Some of the spectra show an intriguing featureless continuum. The redshifts of the off-nuclear emission lines and stellar components are very close to those of the QSOs. In addition, we compare these spectra to Bruzual and Charlot population synthesis models.
NATO Science Series II: Mathematics, Physics and Chemistry, 2006
We present the basics of optical design as it applies to two mirrored telescope systems. We discu... more We present the basics of optical design as it applies to two mirrored telescope systems. We discuss Zernike decomposition of wave-front error and the description of Strehl in terms of small Zernike errors. We also discuss the balancing of aberrations for a two mirror system and present the Ritchey-Chrétien design as an example of a zero coma system.
Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, 2003
We present the design and status report on the development of an Integral Field Unit (IFU) for th... more We present the design and status report on the development of an Integral Field Unit (IFU) for the Echellette spectrograph and imager (ESI), a recently developed R=13000, Cassegrain spectrograph at Keck II. We have designed a family of IFU&amp;quot;s for the spectrograph, providing a range of field-coverages and dispersions. The optical designs are based on the Advanced Image Slicer concept
We present optical spectroscopy of the host galaxies of 4 QSO's: PG 1444+407, PKS 2349-147, 3C 32... more We present optical spectroscopy of the host galaxies of 4 QSO's: PG 1444+407, PKS 2349-147, 3C 323.1, and 4C 31.63 having a redshift range 0.1 ≤ z ≤ 0.3. The spectra were obtained at the Keck Observatory with the LRIS instrument offset 2-4 arcseconds from the nucleus at several position angles in each galaxy. The objects close to 3C 323.1 and PKS 2349-147 have the same redshifts of their nearby QSOs and appear to be the nuclei of galaxies in the final states of merging with the host galaxies. The spectra of the hosts show some variety: PKS 2349-147 and 3C 323.1 show strong off-nuclear emission lines plus stellar absorption features, while the other two show only stellar absorption. PKS 2349-147 and PG 1444+407 have a mixture of old and moderately young stars, while 4C 31.63 has the spectrum of a normal giant elliptical, which is very rare in our larger sample. The spectrum of the host of 3C 323.1 appears to dominated by older stars, though our data for it are of lower quality. The redshifts of the off-nucleus emission lines and stellar components are very close to those of the associated QSOs.
We present stellar velocity dispersion measurements in the host galaxies of 10 luminous quasars (... more We present stellar velocity dispersion measurements in the host galaxies of 10 luminous quasars (M V < −23) using the Ca H&K lines in off-nuclear spectra. We combine these data with effective radii and magnitudes from the literature to place the host galaxies on the Fundamental Plane (FP) where their properties are compared to other types of galaxies. We find that the radio-loud (RL) QSO hosts have similar properties to massive elliptical galaxies, while the radio-quiet (RQ) hosts are more similar to intermediate mass galaxies. The RL hosts lie at the upper extreme of the FP due to their large velocity dispersions ( σ * = 321 km s −1 ), low surface brightness ( µ e (r) = 20.8 mag arcsec −2 ), and large effective radii ( R e = 11.4 kpc), and have M * = 1.5 x 10 12 M ⊙ and M/L = 12.4. In contrast, properties of the RQ hosts are σ * = 241 km s −1 , M * ∼ 4.4 x 10 11 M ⊙ , and M/L ∼ 5.3. The distinction between these galaxies occurs at σ * ∼ 300 km s −1 , R e ∼ 6 kpc, and corresponding M * ∼ 5.9 ± 3.5 x 10 11 M ⊙ . Our data support previous results that PG QSOs are related to gas-rich galaxy mergers that form intermediate-mass galaxies, while RL QSOs reside in massive early-type galaxies, most of which also show signs of recent mergers or interactions. Most previous work has drawn these conclusions by using estimates of the black hole mass and inferring host galaxy properties from that, while here we have relied purely on directly measured host galaxy properties.
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Papers by Andrew Sheinis