Kenneth M. Lanzetta

Stony Brook University

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John K. Webb

University of Cambridge

A. Fernández-Soto

Universitat de València

Hsiao‐Wen Chen

Children's Hospital of Philadelphia

S. M. Pascarelle

In Depth Engineering (United States)

X. Barcons

Instituto de Física de Cantabria

A. Yahil

Stony Brook University

Noriaki Yahata

The University of Tokyo

Arthur M. Wolfe

University of California, San Diego

Michael M. Shara

American Museum of Natural History

Stefan Gromoll

Laboratoire d’Etudes du Rayonnement et de la Matière en Astrophysique et Atmosphères

Cooperative Institutions

California Institute of Technology

Center for Astrophysics Harvard & Smithsonian

University of California, San Diego

Kitt Peak National Observatory

Harvard University

Centre National de la Recherche Scientifique

Goddard Space Flight Center

Association of Universities For Research In Astronomy

U.S. National Science Foundation

Stony Brook University

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The Star Formation Density in the High-Redshift Universe

Springer eBooks (2006)

A. Fernández-Soto Kenneth M. Lanzetta Hsiao‐Wen Chen S. M. Pascarelle Noriaki Yahata

Star (game theory)

10.1007/10854354_34

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Introducing the Condor Array Telescope: IV. A possible nova super-remnant surrounding the putative recurrent nova KT Eridani

arXiv (Cornell University) (2023)

Michael M. Shara Kenneth M. Lanzetta James T. Garland Stefan Gromoll D. Valls‐Gabaud

Just 10 recurrent novae (RNe) - which erupt repeatedly on timescales shorter than one century - are known in our Galaxy. The most extreme RN known (located in the Andromeda galaxy), M31N 2008-12a, undergoes a nova eruption every year, and is surrounded by a vast nova "super-remnant", 134 pc in extent. Simulations predict that all RNe should be surrounded by similar vast shells, but previous searches have failed to detect them. KT Eri has recently been suggested to be a RN, and we have used the Condor Array Telescope to image its environs through multiple narrowband filters. We report the existence of a large ($\sim$ 50 pc diameter), H$\,\alpha$-bright shell centered on KT Eri, exactly as predicted. This strongly supports the claim that KT Eri is the 11th Galactic recurrent nova, and only the second nova known to be surrounded by a super-remnant. SALT spectra of the super-remnant demonstrate that its velocity width is consistent with that of M31-2008-12a.

Nova (rocket)

10.48550/arxiv.2310.17055

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Properties of the very high redshift galaxy population.

Bulletin of the American Astronomical Society (1999)

Kenneth M. Lanzetta

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a Group or Cluster of Ly-Alpha Galaxies at Z ~ 0.26

HST Proposal (1996)

Kenneth M. Lanzetta

Alpha (finance)

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Hydrodynamic simulations of the KT Eridani nova super-remnant

arXiv (Cornell University) (2023)

M. W. Healy-Kalesh M. J. Darnley Michael M. Shara Kenneth M. Lanzetta James T. Garland

A nova super-remnant (NSR) is an immense structure associated with a nova that forms when frequent and recurrent nova eruptions sweep up surrounding interstellar material (ISM) into a high density and distant shell. The prototypical NSR, measuring over 100 pc across, was discovered in 2014 around the annually erupting nova M31N 2008-12a. Hydrodynamical simulations demonstrated that the creation of a dynamic NSR by repeated eruptions transporting large quantities of ISM is not only feasible but that these structures should exist around all novae, whether the white dwarf (WD) is increasing or decreasing in mass. But it is only the recurrent nova (RNe) with the highest WD masses and accretion rates that should host observable NSRs. KT Eridani is, potentially, the eleventh RNe recorded in the Galaxy and is also surrounded by a recently unveiled H{\alpha} shell tens of parsecs across, consistent with a NSR. Through modelling the nova ejecta from KT Eri, we demonstrate that such an observable NSR could form in approximately 50,000 years, which fits with the proper motion history of the nova. We compute the expected H{\alpha} emission from the KT Eri NSR and predict that the structure might be accessible to wide-field X-ray facilities.

Nova (rocket)

10.48550/arxiv.2310.17258

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The Origin of Intermediate-Redshift Lyman Alpha Absorption Systems

arXiv (Cornell University) (1994)

Kenneth M. Lanzetta David V. Bowen David Tytler John K. Webb Katrina Sealey

We present initial results of an imaging and spectroscopic survey of faint galaxies in fields of Hubble Space Telescope spectroscopic target QSOs. The primary objectives of the survey are (a) to determine the incidence, extent, and covering factor of extended gaseous envelopes of luminous galaxies and (b) to determine the fraction of Lyman alpha absorption systems that arise in luminous galaxies. The goal of the survey is to identify in each field under consideration all objects with apparent r-band magnitudes satisfying r< 21.5 within angular distances to the QSOs satisfying theta < 1.3 arcmin. We find that at z \apl 1 most luminous galaxies are surrounded by extended gaseous envelopes of approx 160 h^{-1} kpc radius and roughly unit covering factor and that at z \apl 1 the fraction of Ly alpha absorption systems that arise in luminous galaxies is at least 0.35 \pm 0.10 and is likely 0.65 \pm 0.18.

QSOS

10.48550/arxiv.astro-ph/9410040

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Galaxies at Redshifts z > 5

arXiv (Cornell University) (1998)

Kenneth M. Lanzetta Hsiao‐Wen Chen S. M. Pascarelle Noriaki Yahata

Here we describe our attempts to establish statistically complete samples of very high redshift galaxies by obtaining photometric redshifts of galaxies in Medium Deep Survey (MDS) fields and photometric and spectroscopic redshifts of galaxies in very deep STIS slitless spectroscopy fields. On the basis of this analysis, we have identified galaxies of redshift z = 4.92 in an MDS field and of redshift z = 6.68 in a very deep STIS field.

Red shift

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Properties of a Chemically Enriched Lya Absorption System at z=0.167 and Implications for the Total Baryons in Extended Gaseous Envelopes Around Galaxies

arXiv (Cornell University) (2001)

Hsiao‐Wen Chen J. X. Prochaska Kenneth M. Lanzetta

We present a detailed analysis of the chemical abundances, ionization state, and origin of a partial Lyman limit system (N(HI) ~ 10^{16} cm^{-2}) at low redshift (z=0.167 towards PKS0405-1219). We also present the first estimate of the total baryons in extended gaseous envelopes around galaxies based on a simple photoionization model for the Lya absorbers. We find that extended gaseous envelopes can explain between 5--20% of the total baryons predicted by the big bang nucleosynthesis model.

10.48550/arxiv.astro-ph/0108068

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Galaxies of Redshift z >5: The View from Stony Brook

ASPC (1999)

Kenneth M. Lanzetta H. W. Chen A. Fernández-Soto S. M. Pascarelle Noriaki Yahata

We report on some aspects of our efforts to establish properties of the extremely faint galaxy population by applying our photometric redshift technique to the HDF and HDF-S WFPC2 and NICMOS fields. We find that cosmological surface brightness dimming effects play a dominant role in setting what is observed at redshifts z > 2, that the comoving number density of high intrinsic surface brightness regions increases monotonically with increasing redshift, and that previous estimates neglect a significant or dominant fraction of the ultraviolet luminosity density of the universe due to surface brightness effects. The ultraviolet luminosity density of the universe plausibly increases monotonically with increasing redshift to redshifts beyond z = 5.

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Introducing the Condor Array Telescope. I. Motivation, Configuration, and Performance

Publications of the Astronomical Society of the Pacific (2023)

Kenneth M. Lanzetta Stefan Gromoll Michael M. Shara Stephen Berg D. Valls‐Gabaud

Abstract The “Condor Array Telescope” or “Condor” is a high-performance “array telescope” comprised of six apochromatic refracting telescopes of objective diameter 180 mm, each equipped with a large-format, very low-read-noise (≈1.2 e − ), very rapid-read-time (<1 s) CMOS camera. Condor is located at a very dark astronomical site in the southwest corner of New Mexico, at the Dark Sky New Mexico observatory near Animas, roughly midway between (and more than 150 km from either) Tucson and El Paso. Condor enjoys a wide field of view (2.29 × 1.53 deg 2 or 3.50 deg 2 ), is optimized for measuring both point sources and extended, very low-surface-brightness features, and for broad-band images can operate at a cadence of 60 s (or even less) while remaining sky-noise limited with a duty cycle near 100%. In its normal mode of operation, Condor obtains broad-band exposures of exposure time 60 s over dwell times spanning dozens or hundreds of hours. In this way, Condor builds up deep, sensitive images while simultaneously monitoring tens or hundreds of thousands of point sources per field at a cadence of 60 s. Condor is also equipped with diffraction gratings and with a set of He ii 468.6 nm, [O iii ] 500.7 nm, He i 587.5 nm, H α 656.3 nm, [N ii ] 658.4 nm, and [S ii ] 671.6 nm narrow-band filters, allowing it to address a variety of broad- and narrow-band science issues. Given its unique capabilities, Condor can access regions of “astronomical discovery space” that have never before been studied. Here we introduce Condor and describe various aspects of its performance.

10.1088/1538-3873/acaee6

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Citations (10)