A Three-Position Spectral Line Survey of Sagittarius B2 between 218 and 263 GHz. II. Data Analysis

By A. Nummelin, P. Bergman, Å. Hjalmarson, P. Friberg, William M. Irvine, Thomas J. Millar, Masatoshi Ohishi, S. Saito. 2000

234 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/f0c2fcd9dab0aa8025721e4a6f0c59a8a0453ef6

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Spectroscopy

Citations in the corpus

Erratum: Detection of amino acetonitrile in Sgr B2(N) (2008, background): “They found that water can efficiently catalyze a reaction between methylenimine CH2NH and hydrogen isocyanide HNC to form amino acetonitrile in the grain mantles at a temperature of 50 K. Methylenimine was detected in the gas phase toward Sgr B2(N) by, e.g., Nummelin et al. (2000).”
On the Formation of Glycolaldehyde (HCOCH2OH) and Methyl Formate (HCOOCH3) in Interstellar Ice Analogs (2007, background): “Taking the column density of H2 as 3 ; 10 24 molecules cm 2 (Nummelin et al. 2000), this gives fractional abundances (relative to H2) of 2.0 ; 10 11, 2.0 ; 10 9, and 3.7 ; 10 8 for glycolaldehyde, acetic acid, and methyl formate, respectively.”
Complex Chemistry in Star-forming Regions: An Expanded Gas-Grain Warm-up Chemical Model (2008, background): “The majority of these observational values are derived from the survey by Nummelin et al. (2000).”
A 2 Millimeter Spectral Line Survey of the Starburst Galaxy NGC 253 (2006, methodology): “The existing molecular line surveys toward the Galactic center sources Sgr B2(OH) (Cummins et al. 1986; Turner 1989, 1991) and Sgr B2(N, M, and NW) (Nummelin et al. 1998, 2000) were also used as additional information to estimate the expected intensity of the fainter identified lines not included…”
Testing grain-surface chemistry in massive hot-core regions (2007, background): “The abundance ratios with respect to CH3OH for Sgr B2(N) from Nummelin et al. (2000) appear to be significantly lower than for the sources in our sample.”
Formation rates of complex organics in UV irradiated CH3OH-rich ices I: Experiments (2009, background): “Organic molecules of increasing complexity are being detect d in star-forming regions (Blake et al. 1987; Nummelin et al. 2000; Bisschop et al. 2007b; van Dishoeck et al. 1995; Cazaux et al. 2003; Bottinelli et al. 2004, 2007; Belloche et al. 2009); however, the origins of these complex…”
Hot corinos in NGC 1333-IRAS4B and IRAS2A (2006, methodology): “…is that the abundance ratios in the massive hot cores have been derived by beam-averaged column densities, except for SgrB2 (N) and (M), where Nummelin et al. (2000) have carried out an analysis of the methanol emission similar to what has been done for the hot corinos, namely disentangling…”
Spatially Resolved Chemistry in Nearby Galaxies. I. The Center of IC 342 (2004, background): “CH3OH abundances in the envelope of SgrB2 are 3 − 10 × 10 −9 (Nummelin et al. 2000).”
Complex organic molecules in the interstellar medium: IRAM 30 m line survey of Sagittarius B2(N) and (M) (2013, background): “We refer to Belloche et al. (2009) for a comparison of our fit resultto those obtained by Nummelin et al. (2000).”
The Gas-Phase Formation of Methyl Formate in Hot Molecular Cores (2004, background): “While methyl formate has been found in numerous sources (Ellder et al. 1980; Millar et al. 1997; Nummelin et al. 2000), acetic acid (Mehringer et al. 1997) and glycolaldehyde (Hollis et al. 2000) have been found only in the Sgr B2(N-LMH) source.”
Formation of methyl formate and other organic species in the warm-up phase of hot molecular cores (2006, background): “Various large molecules including methyl formate (HCOOCH3) have been detected in a number of hot molecular cores and corinos (Blake et al. 1987; Hatchell et al. 1998; Nummelin et al. 2000; Cazaux et al. 2003; Bottinelli et al. 2004).”
Increased complexity in interstellar chemistry: detection and chemical modeling of ethyl formate and n-propyl cyanide in Sagittarius B2(N) (2009, methodology): “The discrepancy most likely comes from the beam filling factor of unity assumed by Nummelin et al. (2000) that leads to underestimating the line opacities.”