J. L. Rosenberg

Publications (8)4.9 Total impact

• Source

  Available from: Robert F. Minchin

  Article: The Arecibo L-band Feed Array Zone of Avoidance Survey I: Precursor Observations through the Inner and Outer Galaxy

  P. A. Henning, C. M. Springob, R. F. Minchin, E. Momjian, B. Catinella, T. McIntyre, F. Day, E. Muller, B. Koribalski, J. L. Rosenberg, S. Schneider, L. Staveley-Smith, W. van Driel
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  ABSTRACT: The Arecibo L-band Feed Array (ALFA) is being used to conduct a low-Galactic latitude survey, to map the distribution of galaxies and large-scale structures behind the Milky Way through detection of galaxies' neutral hydrogen (HI) 21-cm emission. This Zone of Avoidance (ZOA) survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially-obscured galaxies known at other wavelengths. Before the commencement of the full survey, two low-latitude precursor regions were observed, totalling 138 square degrees, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have 2MASS counterparts. We present the results of these precursor observations, including a catalog of the detected galaxies, with their HI parameters. The survey sensitivity is well described by a flux- and linewidth-dependent signal-to-noise ratio of 6.5. ALFA ZOA galaxies which also have HI measurements in the literature show good agreement between our measurements and previous work. The inner Galaxy precursor region was chosen to overlap the HI Parkes Zone of Avoidance Survey so ALFA performance could be quickly assessed. The outer Galaxy precursor region lies north of the Parkes sky. Low-latitude large-scale structure in this region is revealed, including an overdensity of galaxies near l = 183 deg and between 5000 - 6000 km/s in the ZOA. The full ALFA ZOA survey will be conducted in two phases: a shallow survey using the observing techniques of the precursor observations, and also a deep phase with much longer integration time, with thousands of galaxies predicted for the final catalog. Comment: 26 pages, 7 figures, 2 tables, Astronomical Journal accepted
  02/2010;
• Article: The ALFA Zone of Avoidance Survey

  P. A. Henning, C. M. Springob, F. Day, R. Minchin, E. Momjian, B. Catinella, E. Muller, B. Koribalski, K. Masters, C. Pantoja, M. Putman, J. L. Rosenberg, S. Schneider, L. Staveley‐Smith
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  ABSTRACT: The Arecibo L‐Band Feed Array (ALFA) Zone of Avoidance (ZOA) team is mapping the distribution of low‐Galactic‐latitude galaxies and large‐scale structures through detection of galaxies'21‐cm emission with ALFA. This ZOA survey finds new HI galaxies which lie hidden behind the Milky Way, and also provides redshifts for partially‐obscured galaxies known at other wavelengths. Two precursor regions which straddle the Galactic plane have been observed to date, totalling 140 square degrees, with 72 HI galaxies detected. Detections through the inner Galaxy generally have no cataloged counterparts in any other waveband, due to the heavy extinction and stellar confusion. Detections through the outer Galaxy are more likely to have 2MASS counterparts, and we provide redshifts for these galaxies. A third region, through the Taurus molecular cloud, has also been observed. The full ALFA ZOA survey will reveal more previously unknown galaxies and map low‐latitude large‐scale structures.
  AIP Conference Proceedings. 07/2008; 1035(1):246-248.
• Source

  Available from: Robert F. Minchin

  Article: The Arecibo Galaxy Environment Survey: II. A HI view of the Abell cluster 1367 and its outskirts

  L. Cortese, R. F. Minchin, R. R. Auld, J. I. Davies, B. Catinella, E. Momjian, J. L. Rosenberg, R Taylor, G. Gavazzi, K. O'Neil, M. Baes, A. Boselli, G. Bothun, B. Koribalski, S. Schneider, W. van Driel
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  ABSTRACT: We present 21 cm HI line observations of 5x1 square degrees centered on the local Abell cluster 1367 obtained as part of the Arecibo Galaxy Environment Survey. One hundred sources are detected (79 new HI measurements and 50 new redshifts), more than half belonging to the cluster core and its infalling region. Combining the HI data with SDSS optical imaging we show that our HI selected sample follows scaling relations similar to the ones usually observed in optically selected samples. Interestingly all galaxies in our sample appear to have nearly the same baryon fraction independently of their size, surface brightness and luminosity. The most striking difference between HI and optically selected samples resides in their large scale distribution: whereas optical and X-ray observations trace the cluster core very well, in HI there is almost no evidence of the presence of the cluster. Some implications on the determination of the cluster luminosity function and HI distribution for samples selected at different wavelength are also discussed. Comment: 22 pages, 15 figures, 4 tables. Accepted for publication on MNRAS Main Journal. High resolution version of this paper can be downloaded at http://www.astro.cf.ac.uk/pub/Luca.Cortese/papers/ages_a1367.pdf . Datacubes and catalogs can be downloaded at http://www.naic.edu/~ages/public_data.html
  11/2007;
• Source

  Available from: Robert F. Minchin

  Article: The ALFA Zone of Avoidance Survey: Results from the Precursor Observations

  C. M. Springob, P. A. Henning, B. Catinella, F. Day, R. Minchin, E. Momjian, B. Koribalski, K. L. Masters, E. Muller, C. Pantoja, M. Putman, J. L. Rosenberg, S. Schneider, L. Staveley-Smith
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  ABSTRACT: The Arecibo L-band Feed Array Zone of Avoidance Survey (ALFA ZOA) will map 1350-1800 square degrees at low Galactic latitude, providing HI spectra for galaxies in regions of the sky where our knowledge of local large scale structure remains incomplete, owing to obscuration from dust and high stellar confusion near the Galactic plane. Because of these effects, a substantial fraction of the galaxies detected in the survey will have no optical or infrared counterparts. However, near infrared follow up observations of ALFA ZOA sources found in regions of lowest obscuration could reveal whether some of these sources could be objects in which little or no star formation has taken place ("dark galaxies"). We present here the results of ALFA ZOA precursor observations on two patches of sky totaling 140 square degrees (near l=40 degrees, and l=192 degrees). We have measured HI parameters for detections from these observations, and cross-correlated with the NASA/IPAC Extragalactic Database (NED). A significant fraction of the objects have never been detected at any wavelength. For those galaxies that have been previously detected, a significant fraction have no previously known redshift, and no previous HI detection. Comment: To appear in Proceedings of IAU Symp #244, "Dark Galaxies and Lost Baryons", June 2007, 2 pages, including 1 figure
  08/2007;
• Source

  Available from: Noah Brosch

  Article: The Arecibo Legacy Fast ALFA Survey: III. HI Source Catalog of the Northern Virgo Cluster Region

  R. Giovanelli, M. P. Haynes, B. R. Kent, A. Saintonge, S. Stierwalt, A. Altaf, T. Balonek, N. Brosch, S. Brown, B. Catinella, [......], R. A. Koopmann, D. A. Kornreich, B. Mahmood, A. M. Martin, K. L. Masters, A. Mitschang, E. Momjian, P. H. Nair, J. L. Rosenberg, B. Walsh
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  ABSTRACT: We present the first installment of HI sources extracted from the Arecibo Legacy Fast ALFA (ALFALFA) extragalactic survey, initiated in 2005. Sources have been extracted from 3-D spectral data cubes and then examined interactively to yield global HI parameters. A total of 730 HI detections are catalogued within the solid angle 11h44m < R.A.(J2000) < 14h00m and +12deg < Dec.(J2000) < +16deg, and redshift range -1600 \kms < cz < 18000 \kms. In comparison, the HI Parkes All-Sky Survey (HIPASS) detected 40 HI signals in the same region. Optical counterparts are assigned via examination of digital optical imaging databases. ALFALFA HI detections are reported for three distinct classes of signals: (a) detections, typically with S/N > 6.5; (b) high velocity clouds in the Milky Way or its periphery; and (c) signals of lower S/N (to ~ 4.5) which coincide spatially with an optical object of known similar redshift. Although this region of the sky has been heavily surveyed by previous targeted observations based on optical flux-- or size-- limited samples, 69% of the extracted sources are newly reported HI detections. The resultant positional accuracy of HI sources is 20" (median). The median redshift of the sample is ~7000 \kms and its distribution reflects the known local large scale structure including the Virgo cluster. Several extended HI features are found in the vicinity of the Virgo cluster. A small percentage (6%) of HI detections have no identifiable optical counterpart, more than half of which are high velocity clouds in the Milky Way vicinity; the remaining 17 objects do not appear connected to or associated with any known galaxy.
  03/2007;
• Source

  Available from: Robert F. Minchin

  Article: The Arecibo Galaxy Environment Survey: precursor observations of the NGC 628 group

  R. Auld, R. F. Minchin, J. I. Davies, B. Catinella, W. Van Driel, P. A. Henning, S. Linder, E. Momjian, E. Muller, K. O'Neil, [......], M. Baes, W. J. G. De Blok, A. Boselli, E. Brinks, N. Brosch, J. Irwin, I. D. Karachentsev, V. A. Kilborn, B. Koribalski, K. Spekkens
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  ABSTRACT: The Arecibo Galaxy Environment Survey (AGES) is one of several H i surveys utilizing the new Arecibo L-band Feed Array (ALFA) fitted to the 305-m radio telescope at Arecibo.† The survey is specifically designed to investigate various galactic environments to higher sensitivity, higher velocity resolution and higher spatial resolution than previous fully sampled, 21-cm multibeam surveys. The emphasis is on making detailed observations of nearby objects although the large system bandwidth (100 MHz) will allow us to quantify the H i properties over a large instantaneous velocity range.In this paper, we describe the survey and its goals and present the results from the precursor observations of a 5 × 1-deg2 region containing the nearby (∼10 Mpc) NGC 628 group. We have detected all the group galaxies in the region including the low-mass (MH I∼107 M⊙) dwarf, dw0137+1541. The fluxes and velocities for these galaxies compare well with previously published data. There is no intragroup neutral gas detected down to a limiting column density of 2 × 1018 cm−2.In addition to the group galaxies we have detected 22 galaxies beyond the NGC 628 group, nine of which are previously uncatalogued. We present the H i data for these objects and also SuperCOSMOS images for possible optical galaxies that might be associated with the H i signal. We have used V/Vmax analysis to model how many galaxies beyond 1000 km s−1 should be detected and compare this with our results. The predicted number of detectable galaxies varies depending on the H i mass function (HIMF) used in the analysis. Unfortunately the precursor survey area is too small to determine whether this is saying anything fundamental about the HIMF or simply highlighting the effect of low number statistics. This is just one of many questions that will be addressed by the complete AGES survey.
  Monthly Notices of the Royal Astronomical Society 09/2006; 371(4):1617 - 1640. · 4.90 Impact Factor
• Article: Surveying The Zone Of Avoidance With The Arecibo L-band Feed Array

  Patricia A. Henning, C. M. Springob, B. Catinella, E. Momjian, B. Koribalski, K. Masters, E. Muller, C. Pantoja, M. Putman, J. L. Rosenberg, S. Schneider, L. Staveley-Smith
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  ABSTRACT: We are conducting 21-cm surveys with the Arecibo L-Band Feed Array, searching for HI galaxies at low galactic latitudes, where optical obscuration and infrared confusion preclude the mapping of galaxies and large-scale structures in those wavebands. Galaxies which contain HI are detected by these blind surveys, and their Doppler shifted emission locates them in 3 dimensions.The first survey will be of the inner Galaxy accessible to Arecibo (l=30-75 degrees), within 10 degrees of the Galactic equator, and will be relatively shallow (effective integration time of 8-10 seconds per beam, with rms about 6 mJy). We have completed two small regions using this observing mode (near l=40 degrees, and l=192 degrees). The catalog of HI detections will be presented, and future expectations for the full survey will be discussed.We will also be conducting very deep, pointed observations, with dwell times expected to be more than 260 seconds per pointing, over all longitudes accessible to Arecibo. Our expectations for this very deep low Galactic latitude survey will be presented. Both the shallow and deep surveys are conducted in "commensal" modes with other surveys on the telescope, a Galactic HI survey, and a pulsar survey, respectively.P.A.H. acknowledges support from NSF grant AST-0506676.
  05/2006; 38:133.
• Source

  Available from: ArXiv

  Article: The Nearby Damped Lyman-alpha Absorber SBS 1543+593: A Large HI Envelope in a Gas-Rich Galaxy Group

  J. L. Rosenberg, D. V. Bowen, T. M. Tripp, E. Brinks
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  ABSTRACT: We present a Very Large Array (VLA) HI 21cm map and optical observations of the region around one of the nearest damped Lyman-alpha absorbers beyond the local group, SBS 1543+593. Two previously uncataloged galaxies have been discovered and a redshift has been determined for a third. All three of these galaxies are at the redshift of SBS 1543+593 and are ~185 kpc from the damped Lyman-alpha absorber. We discuss the HI and optical properties of SBS 1543+593 and its newly identified neighbors. Both SBS 1543+593 and Dwarf 1 have baryonic components that are dominated by neutral gas -- unusual for damped Lyman-alpha absorbers for which only ~5% of the HI cross-section originates in such strongly gas-dominated systems. What remains unknown is whether low mass gas-rich groups are common surrounding gas-rich galaxies in the local universe and whether the low star-formation rate in these systems is indicative of a young system or a stable, slowly evolving system. We discuss these evolutionary scenarios and future prospects for answering these questions.
  05/2006;