arXiv subjects

R. Lucas

Publications and source records attributed to R. Lucas.

27 records · Page 2Linked to original sources

arXiv2004

Mm-wave HCO+, HCN and CO absorption toward NGC1052

We used the Plateau de Bure Interferometer to observe $λ$3mm J=1-0 absorption lines of \hcop, HCN and CO toward the core of the nearby elliptical, megamaser-host galaxy NGC1052. The lines are relatively weak, with peak optical depths 0.03 for \hcop and HCN and 0.1 for CO. Nonetheless the inferred column density of molecular gas 2N(\HH) $\simeq 5\times10^{21}~\pcc$ is consistent with the degree of reddening inferred toward the nucleus from observations of the Balmer series of hydrogen. Mm-wave absorption line profiles are somewhat broader than those of H I and OH, perhaps because lower free-free opacity at mm-wavelengths exposes higher-velocity material nearer the nucleus. Overall, the OH/\hcop ratio in NGC1052 is as expected from the strong relationship established in local diffuse clouds but the optical depth ratio varies strongly over the line profiles. Similar variations are also seen toward Cen A, which has very different line ratios among H I, OH and \hcop for very nearly the same amount of OH absorption.

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arXiv2004

The abundance of HOC+ in diffuse clouds

We used the Plateau de Bure Interferometer to search for $λ$3mm absorption lines of HOC+ from local diffuse and translucent clouds occulting compact extragalactic mm-wave continuum sources. We detected HOC+ in three directions with column densities only 70-120 times below those of the HCO+ isomer, a factor 5-50 higher than typically found in dense dark gas but comparable to recent observations of dense photon-dominated regions. The observed amounts of HOC+, N(HOC+)/N(\HH) $ = 3-6\times 10^{-11} $, can be made in quiescent diffuse gas at thermal gas-kinetic rates if the {\HH O}/OH ratio is of order unity, in mild violation of extant observational limits. %

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arXiv2004

The Hubble Higher-Z Supernova Search: Supernovae to z=1.6 and Constraints on Type Ia Progenitor Models

We present results from the Hubble Higher-z Supernova Search, the first space-based open field survey for supernovae (SNe). In cooperation with the Great Observatories Origins Deep Survey, we have used the Hubble Space Telescope with the Advanced Camera for Surveys to cover 300 square arcmin in the area of the Chandra Deep Field South and the Hubble Deep Field North on five separate search epochs (separated by 45 day intervals) to a limiting magnitude of z'=26. These deep observations have allowed us to discover 42 SNe in the redshift range 0.2 < z < 1.6. As these data span a large range in redshift, they are ideal for testing the validity of Type Ia supernova progenitor models with the distribution of expected ``delay times,'' from progenitor star formation to SN Ia explosion, and the SN rates these models predict. Through a Bayesian maximum likelihood test, we determine which delay-time models best reproduce the redshift distribution of SNe Ia discovered in this survey. We find that models that require a large fraction of ``prompt'' (less than 2 Gyr) SNe Ia poorly reproduce the observed redshift distribution and are rejected at 95% confidence. We find that Gaussian models best fit the observed data for mean delay times in the range of 3 to 4 Gyr.

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arXiv2003

The Evolution of Early-type Field Galaxies Selected from a NICMOS Map of the Hubble Deep Field North

The redshift distribution of well-defined samples of distant early-type galaxies offers a means to test the predictions of monolithic and hierarchical galaxy formation scenarios. NICMOS maps of the entire Hubble Deep Field North in the F110W and F160W filters, when combined with the available WFPC2 data, allow us to calculate photometric redshifts and determine the morphological appearance of galaxies at rest-frame optical wavelengths out to z ~ 2.5. Here we report results for two subsamples of early-type galaxies, defined primarily by their morphologies in the F160W band, which were selected from the NICMOS data down to H160_{AB} < 24.0. The observed redshift distributions of our two early-type samples do not match that predicted by a monolithic collapse model, which shows an overabundance at z > 1.5. A hierarchical formation model better matches the redshift distribution of the HDF-N early-types at z > 1.5, but still does not adequately describe the observed early-types. The hierarchical model predicts significantly bluer colors on average than the observed early-type colors, and underpredicts the observed number of early-types at z < 1. [abridged]

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arXiv2002

Comparative Chemistry of Diffuse Clouds IV: CH

We observed the 3335 MHz (9cm) F=1-1 line of CH toward a sample of diffuse clouds occulting compact extragalactic mm-wave continuum sources, using the old NRAO 43m telescope. Because radiofrequency observations of CH really must be calibrated with reference to a known CH abundance, we begin by deriving the relationships between CH, EB-V, H2 and other hydrides found by optical spectroscopy. No simple relationship exists between N(CH) and EB-V, since N(CH) is strongly bimodal with respect to reddening for EB-V < 0.3 mag and the typical range in the N(CH)/EB-V ratio is an order of magnitude or more at any given EB-V > 0.3 mag. However, N(CH)/N(H2) = 4.3 +/- 1.9 x 10^-8 in the mean and N(CH) varies as N(H2)^(1.00+/-0.06) for 10^{19} < N(H2) < 10^{21} cm^-2. If CH is a good predictor of H2, 40-45% of the hydrogen in the local diffuse/translucent ISM is in the molecular form at the accepted mean density, higher than previous estimates found in samples of lower-than-average mean density. Optical observations of the population ratios in the upper and lower halves of the CH lambda-doublet suggest that the brightness of the 3335 MHz CH line should be double-valued at a given CH column density in diffuse gas: double-valuedness is noticeable in our data when comparing CH with CO or HCO+. The CH brightness at 3335 MHz is mildly bimodal with respect to CO emission in our diffuse cloud data but much more strongly bimodal when comparing diffuse or translucent gas and dark gas. The CH Lambda-doublet is generally inverted in diffuse gas but we did not succeed in measuring the excitation temperature except toward 3C123 where we confirm one older value Tex ~ -10 K.

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arXiv2002

Comparative chemistry of diffuse clouds III: sulfur-bearing molecules

Using data from IRAM's Plateau de Bure Interferometer and 30 m Telescope, we discuss the mm-wave absorption lines of CS, SO, H2S and HCS+ which arise in diffuse clouds occulting several extragalactic continuum sources. Typical relative abundances are X(CS)/X(HCO+) ~ 2, X(CS)/X(SO) ~ 2, X(CS)/X(H2S) ~ 6 and X(CS)/X(HCS+) ~ 13.

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arXiv2001

Ultraluminous Infrared Galaxies: Atlas of Near-Infrared Images

A sample of 27 ultraluminous infrared galaxy (ULIRG) systems has been imaged at 1.6 microns using the HST Near Infrared Camera and Multi-Object Spectrometer (NICMOS). These ULIRGs are from a larger sample also imaged with HST in the I-band. Images and catalog information for the NICMOS subsample, as well as brief morphological descriptions of each system are presented. Inspection of the infrared images and a comparison with optical images of these systems shows that at least 85% are obviously composed of two or more galaxies involved in a close interaction or merger event, with as many as 93% showing some signs of interaction history. Approximately 37% of the systems show either spectroscopic or morphological characteristics of an active galactic nucleus (AGN). The infrared morphologies of these systems are generally less complicated or disturbed than their optical morphologies, indicating that some of the small-scale features seen in optical images are likely due to complicated patterns of dust obscuration, as well as widely distributed star formation activity. In some systems the high-resolution HST infrared images have revealed nuclear remnants that are obscured or unidentified in ground-based imaging, which has led to changes in previously determined interaction stage classifications or system content. In general, however, the NICMOS images support previous conclusions from previous HST optical imaging.

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arXiv2001

Comparative Chemistry of Diffuse Clouds II: CN, HCN, HNC, CH3CN & N2H+

Using the Plateau de Bure interferometer, we observed the 3mm absorption lines of CN, HCN and HNC from some of the diffuse clouds which lie toward our well-studied sample of compact extragalactic mm-wave continuum sources. The column densities of these species all vary by a factor of about fifty and are prominent in only a limited subset of the clouds seen in the most ubiquitous species such as OH, HCO+, C2H and C3H2. The CN, HCN, and HNC column densities vary in fixed proportion to each other, with = 0.21+/-0.05 and = 6.8+/-1. We searched unsuccessfully for CH3CN and N2H+, which are underabundant compared to dark clouds, by factors of at least 10 and 100, respectively.

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arXiv1998

29SiO (v=0) and 28SiO (v=1) J=2-1 maser emission from Orion IRc2

We have observed with the IRAM interferometer at two different epochs and simultaneously the two transitions v=0, J=2-1 and v=1, J=2-1 of 29SiO and 28SiO in Orion IRc2. We have made the first maps of 29SiO v=0, J=2-1 emission from Orion. These maps and properties of the 29SiO spectra attest to maser emission. Our 28SiO maps show the stable ring of maser spots observed in previous works. Combining our own data with published works we derive that the relative motion between the two ridges of the 28SiO emission ring is less than about 0.7 AU/yr over a period of 7 years. On the other hand, the weak high velocity maser features observed around 30 km/s seem to move with respect to the stable ring of 28SiO main emission. Our relative 29SiO (v=0) and 28SiO (v=1) spot maps show that most 29SiO and 28SiO emission features are closely related but have not the same spatial extent. We conclude that these masers are not excited in the same gas layers in agreement with pumping models which predict that various v state masers peak in different spatial regions. In addition, our maps of v=0 and v=1 emission suggest that local line overlaps due to turbulence and high gas temperature do not play a dominant role in the excitation of 28SiO and 29SiO, although excitation effects resulting from the overlap of Doppler-shifted ro-vibrational lines may still be significant.

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