A5032352285- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Astronomy and Astrophysical Research
- Galaxies: Formation, Evolution, Phenomena
- Astronomical Observations and Instrumentation
- Atmospheric Ozone and Climate
- Spectroscopy and Laser Applications
- Astro and Planetary Science
- Astrophysical Phenomena and Observations
- Atomic and Molecular Physics
- Radio Astronomy Observations and Technology
- Gamma-ray bursts and supernovae
- Molecular Spectroscopy and Structure
- Superconducting and THz Device Technology
- History and Developments in Astronomy
- Solar and Space Plasma Dynamics
- Astrophysics and Cosmic Phenomena
- Particle Detector Development and Performance
- Nuclear Physics and Applications
- Ionosphere and magnetosphere dynamics
- Adaptive optics and wavefront sensing
- Dark Matter and Cosmic Phenomena
- History and advancements in chemistry
- Radio Wave Propagation Studies
- X-ray Spectroscopy and Fluorescence Analysis
National Radio Astronomy Observatory
2008-2023
U.S. National Science Foundation
1991
Associated Universities, Inc.
1991
The University of Texas at Austin
1972-1987
McDonald's (United States)
1978
Columbia University
1969-1972
Lawrence Berkeley National Laboratory
1967-1969
University of California, Berkeley
1967-1969
The Early Universe Molecular Emission Line Galaxies (EMGs) are a population of galaxies with only 36 examples that hold great promise for the study galaxy formation and evolution at high redshift. classification, luminosity molecular line emission, mass, far-infrared (FIR) luminosity, star efficiency, morphology, dynamical mass currently known sample presented discussed. rates derived from FIR range about 300 to 5000 M(sun)per year 4 x 10^9 1 10^{11} M(sun). At lower end, these rates, gas...
ALMA Cycle 2 observations of the long wavelength dust emission in 145 star-forming galaxies are used to probe evolution ISM. We also develop physical basis and empirical calibration (with 72 low-z z ~ galaxies) for using continuum as a quantitative interstellar medium (ISM) masses. The with highest star formation rates (SFRs) at <z> = 2.2 4.4 have gas masses up 100 times that Milky Way mass fractions reaching 50 80%, i.e. 1 - 4 their stellar find single high-z law: SFR 35 M_ mol^0.89 x...
The use of submillimeter dust continuum emission to probe the mass interstellar and gas in galaxies is empirically calibrated using samples local star-forming galaxies, Planck observations Milky Way, high-redshift galaxies. All these objects suggest a similar calibration, strongly supporting view that Rayleigh–Jeans tail can be used as an accurate very fast medium (ISM) We present ALMA Cycle 0 Band 7 (350 GHz) 107 from z = 0.2 2.5. Three with total 101 were stellar-mass-selected COSMOS have...
Observations have revealed prodigious amounts of star formation in starburst galaxies as traced by dust and molecular emission, even at large redshifts. Recent work shows that for both nearby spiral distant starbursts, the global rate, indicated infrared luminosity, has a tight almost linear correlation with amount dense gas luminosity HCN. Our surveys Galactic cores HCN 1-0 emission show this continues to much smaller scale, nearly same ratio found over 7-8 orders magnitude L_IR, lower...
We report the detection of CO(J = 1→0) emission in strongly lensed high-redshift quasars IRAS F10214+4724 (z 2.286), Cloverleaf 2.558), RX J0911+0551 2.796), SMM J04135+10277 2.846), and MG 0751+2716 3.200), using Expanded Very Large Array Green Bank Telescope. lensing-corrected line luminosities L'CO (0.34–18.4) × 1010 K km s−1 pc2 total molecular gas masses M(H2) (0.27–14.7) M☉ for sources our sample. Based on CO ratios relative to previously reported observations J ⩾ 3 rotational...
ALMA observations of the long wavelength dust continuum are used to estimate interstellar medium (ISM) masses in a sample 708 galaxies at z = 0.3 4.5 COSMOS field. The galaxy has known far-infrared luminosities and, hence, star formation rates (SFRs), and stellar (M$_{\rm *}$) from optical-infrared spectrum fitting. SFRs main sequence (MS) 50 times above MS. derived ISM determine dependence gas mass on redshift, M$_{\rm *}$, specific SFR (sSFR) relative increase approximately 0.63 power rate...
We present 90 mas (37 pc) resolution ALMA imaging of Arp 220 in the CO (1-0) line and continuum at $\lambda = 2.6$ mm. The internal gas distribution kinematics both galactic nuclei are well-resolved for first time. In West nucleus, major dust emission extends out to 0.2\arcsec radius (74 pc); central element shows a strong peak but factor 3 dip emission. this is apparently optically thick ($\tau_{\rm 2.6mm} \sim1$) mm with brightness temperature $\sim147$ K. column ISM nucleus $\rm N_{H2}...
We examine the black hole mass - galaxy bulge relationship in high-redshift QSOs. Black masses are derived from broad emission lines, and host stellar velocity dispersion sigma is estimated widths of radio CO lines. At redshifts z > 3, line narrower than expected for mass, indicating that these giant holes reside undersized bulges by an order magnitude or more. The largest (above 10^9 solar masses) evidently grow rapidly early universe without commensurate growth their galaxies. offer a...
We present a detailed analysis of the relation between infrared luminosity and molecular line luminosity, for variety transitions, using sample 34 nearby galaxies spanning broad range luminosities (10^{10} < L_{IR} 10^{12.5} L_sun). show that power-law index is sensitive to critical density gas tracer used, dominant driver in observed ratios density. As most ultraluminous (ULIRGs) exhibit strong signatures active galactic nuclei (AGN) their center, we revisit previous claims questioning...
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We present here the sensitive HCN (1-0) observations made with VLA of two submillimeter galaxies and QSOs at high redshift. emission is signature dense molecular gas found in giant cloud (GMC) cores, actual sites massive star formation. have first detection a galaxy, SMM J16359+6612. The seen signal-to-noise ratio 4 σ appears to be resolved as double source ≲2'' separation. Our new observations, combined previous detections upper limits, show that FIR/HCN ratios these high-redshift sources...
view Abstract Citations (162) References (21) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Molecular abundance variations in interstellar clouds. Wootten, A. ; Evans, N. J., II Snell, R. vanden Bout, P. The abundances of several molecular species have been obtained for 13 regions a variety were by establishing temperature and density model the through use CO H2CO observations. Then HCO(+), H2CO, HNC, HCN, (C-13)O determined comparing with observed lines....
Abstract Atacama Large Millimeter/submillimeter Array (ALMA) observations of the long-wavelength dust continuum are used to estimate gas masses in a sample 708 star-forming galaxies at z = 0.3−4.5. We determine dependence and star formation efficiencies (SFEs; SFR per unit mass) on redshift (z), M * , rate (SFR) relative main sequence (MS). find that 70% increase SFRs MS is due increased earlier epochs, while 30% efficiency (SF). For above this reversed—with being elevated SFEs. Thus, major...
view Abstract Citations (44) References (8) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Laboratory measurements and a search for interstellar CO dimer. Vanden Bout, P. A. ; Steed, J. M. Bernstein, L. S. Klemperer, W. Five laboratory radio-frequency transitions observed the dimer of carbon monoxide are reported. The species (CO)2 appears to be nonrigid. No emission was detected in 11 sources at 1.458 GHz. It is estimated that ratio (CO)2/CO less than 1%...
Three one-dimensional area-scanning photometers under computer control, equipped to observe in one color, were taken observing stations Australia, India, and Africa the occultation of Beta Scorpii system by Jupiter on 13 May 1971. Six high-quality light curves obtained; three occulta- tions brighter component Sco A C. The mean scale height Jovian upper atmosphere is 32+6 km near - 100 zenographic latitude, 31+2 at 470 24+2 570 latitude. determination atmospheric highly sensitive background...
We have measured the hyperfine-structure separations and nuclear magnetic moments of (2.70-day) ${\mathrm{Au}}^{198}$ (3.15-day) ${\mathrm{Au}}^{199}$ in $^{2}S_{\frac{1}{2}}$ state, using atomic-beam magnetic-resonance method. also ratios electronic $g$ factor gold to those potassium cesium. The results are, for ${\mathrm{Au}}^{198} (I=2)$, $\ensuremath{\Delta}\ensuremath{\nu}=21450.7167(4)$ MHz, ${\ensuremath{\mu}}_{I}(\mathrm{uncorr})=+0.5842(4)$ nm; ${\mathrm{Au}}^{199} (I=\frac{3}{2})$,...
X-ray emission from the Cygnus Loop was observed in energy region around 0.2 to 1 kiloelectronvolt with a collector that focused x-rays along one dimension while scanning across nebula. The total integrated intensity is 1.3x 10(-8) erg per square centimeter second. one-dimensional x-ray structure has same angular size-about 3 degrees-as outermost boundaries of optical filaments. There no increase at center nebula nor strong feature seen certain radio maps. spectrum consistent thermal...
An x-ray polarimeter sensitive to x rays in the energy range from 6 18 keV, flown above atmosphere on 27 July 1968, was used both set an upper limit polarization of Sco X-1 and check for spurious indications which might result anisotropy cosmic rays. Within statistical limitations data, no evidence found background polarization.
view Abstract Citations (74) References (10) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS IRAS F10214+4724: an Extended CO Emission Source at Z = 2.2867 Brown, Robert L. ; Vanden Bout, Paul A. Using the IRAM 30 m telescope, we observed CO(J 3-2) and 4-3) emission lines z from gas-rich protogalaxy F10214+4724. We estimate molecular mass to be 3 x 10^11^ h^-2^< MJ(H_2_)/M_sun_ <3 10^12^ h^-2^ gas-to-dust ratio as 1500 < M(H_2_)/M_d_ 15,000. A comparison of...
We report the detection of HCO+ (5-4) emission from broad absorption line quasar APM 08279+5255 at z = 3.911 based on observations conducted with IRAM Plateau de Bure Interferometer. This represents first this molecular ion such a high redshift. The inferred luminosity, uncorrected for lensing, is L (3.5 ± 0.6) × 1010 K km s-1 pc2. J 5-4 source position coincides within errors that reported previous HCN and high-J CO quasar. profile central velocity width are consistent those derived HCN....
view Abstract Citations (143) References (22) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS The energetics of molecular clouds. II - S140 cloud Blair, G. N. ; Evans, J., Vanden Bout, P. A. Peters, W. L., III Techniques analysis which allow estimates kinetic temperature, gas density, cooling rate, and dust rate are applied to the cloud. Maps this in various lines examined reveal existence a strong temperature density peak near H-alpha rim presence near-IR...
We present observations made with the 10 m Heinrich Hertz Submillimeter Telescope of HCN(3-2) emission from a sample 30 nearby galaxies ranging in infrared luminosity 1010 to 1012.5 L☉ and 106 109 K km s−1 pc2. examine correlation between find that best-fit linear regression has slope (in log-log space) 0.74 ± 0.12. Including recently published data Graciá-Carpio et al. tightens constraints on 0.79 0.09. This below unity suggests molecular line is not linearly tracing amount dense gas. Our...
view Abstract Citations (96) References (35) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Simultaneous ultraviolet, optical and X-ray observations of the X-raysource Vel X-1 (HD 77581). Dupree, A. K. ; Gursky, H. Black, J. Davis, R. Hartmann, L. Matilsky, T. Raymond, C. Hammerschlag-Hensberge, G. van den Heuvel, E. P. Burger, M. Lamers, Vanden Bout, Morton, D. De Loore, Dessel, Menzies, W. Whitelock, Watson, Sanford, Pollard, S. UV spectra (obtained by...
We have measured the ratios of electronic $g$ factors $^{23}\mathrm{Na}$, $^{85,87}\mathrm{Rb}$, and $^{133}\mathrm{Cs}$ to that $^{39}\mathrm{K}$, using atomic-beam magnetic-resonance technique. The results are $\frac{{g}_{J}(^{23}\mathrm{Na})}{{g}_{J}(^{39}\mathrm{K})}=1.0000007(2)$, $\frac{{g}_{J}(^{85,87}\mathrm{Rb})}{{g}_{J}(^{39}\mathrm{K})}=1.0000182(2)$, $\frac{{g}_{J}(^{1333}\mathrm{Cs})}{{g}_{J}(^{39}\mathrm{K})}=1.0001231(3)$. These results, combined with other researchers, yield...