1.1.2 gamma + d -&gt; gamma + d

Genzel, H.; Pfeil, W.

doi:10.1007/10201137_3

Cited by 13 publications

(17 citation statements)

References 1 publication

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“…This argument assumes that the characteristic field inferred from the DCF technique is approximately uniform over the BN/KL region. Zeeman measurements of H 2 O masers have indicated fields up to ∼40 mG near the infrared source IRc2 near the center of the BN/KL region (Genzel & Downes 1977;Garay et al 1989;Fiebig & Guesten 1989) indicating that the details of the magnetic interaction are more complicated than the simple picture presented here. However, these large fields are likely confined to very small volumes of high density material and unlikely to significantly affect the dynamics in the volumes discussed here.…”

Section: The Bn/kl Explosionmentioning

confidence: 67%

HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1

Chuss

Andersson

Bally

et al. 2019

ApJ

100

130

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Section: The Bn/kl Explosionmentioning

confidence: 67%

HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1

Chuss

Andersson

Bally

et al. 2019

ApJ

100

130

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“…MonR2 contains several sites of star formation (see Carpenter & Hodapp 2008, and references therein). The MonR2 clump (size of ∼3 ′ or 0.7 pc) has a mass of 1800 M ⊙ (Ridge et al 2003) and is the most active star forming region in the MonR2 complex as revealed by the blister-type HII region (Massi et al 1985;Wood & Churchwell 1989), the dense stellar cluster (Carpenter et al 1997;Kohno et al 2002), the large-scale CO outflow (one of the largest -∼0.6-7 pc -and most massive -275 M ⊙reported so far; Loren 1981;Wolf et al 1990;Tafalla et al 1997), and the H 2 O and OH masers found in this region (Downes et al 1975;Genzel & Downes 1977;Smits et al 1998). Among the IR sources detected in the cluster (Carpenter et al 1997), the sources IRS1, IRS2 and IRS3 are the most luminous objects in the MonR2 region, with luminosities of 3000 L ⊙ , 6000 L ⊙ and 15000 L ⊙ respectively (Henning et al 1992).…”

Section: Introductionmentioning

confidence: 99%

Submillimeter Array High-Angular Resolution Observations of the Monoceros R2 Star-Forming Cluster

Dierickx

Jiménez-Serra

Rivilla

et al. 2015

ApJ

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We present the first high-angular resolution study of the MonR2 star-forming complex carried out with the Submillimeter Array at (sub-)millimeter wavelengths. We image the continuum and molecular line emission toward the young stellar objects in MonR2 at 0.85 mm and 1.3 mm, with resolutions ranging from 0.5" to ∼ 3". While freefree emission dominates the IRS1 and IRS2 continuum, dust thermal emission prevails for IRS3 and IRS5, giving envelope masses of ∼0.1-0.3 M ⊙ . IRS5 splits into at least two sub-arcsecond scale sources, IRS5B and the more massive IRS5A. Our 12 CO(2-1) images reveal 11 previously unknown molecular outflows in the MonR2 clump. Comparing these outflows with known IR sources in the IRS5 and IRS3 subclusters allows for tentative identification of driving stars. Line images of molecular species such as CH 3 CN or CH 3 OH show that, besides IRS3 (a well-known hot molecular core), IRS5 is also a chemically active source in the region. The gas excitation temperature derived from CH 3 CN lines toward IRS5 is 144 ± 15 K, indicating a deeply embedded protostar at the hot-core evolutionary stage. SED fitting of IRS5 gives a mass of ∼7 M ⊙ and a luminosity of 300 L ⊙ for the central source. The derived physical properties of the CO outflows suggest that they contribute to the turbulent support of the MonR2 complex and to the gas velocity dispersion in the clump's center. The detection of a large number of CO outflows widespread across the region supports the competitive accretion scenario as origin of the MonR2 star cluster.

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“…All the velocity components in the HOPS 64 spectrum may be attributed to the Orion KL masers, and no H 2 O maser associated specifically with HOPS 64 was detected in this survey. Detections of an H 2 O maser in this region, however, were reported previously (Morris & Knapp 1976;Genzel & Downes 1979). Interferometric observations showed that the H 2 O maser is associated with FIR 3 (Tofani et al 1995).…”

Section: Klc 1 In the Hops 64 Field (Omc 2)mentioning

confidence: 72%

Water and Methanol Maser Survey of Protostars in the Orion Molecular Cloud Complex

Kang

Lee

Choi

et al. 2013

ApJS

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The results of a maser survey toward ninety-nine protostars in the Orion molecular cloud complex are presented. The target sources are low-mass protostars identified from infrared observations. Single-dish observations were carried out in the water maser line at 22 GHz and the methanol class I maser lines at 44, 95, and 133 GHz. Most of the detected sources were mapped to determine the source positions. Five water maser sources were detected, and they are excited by HH 1-2 VLA 3, HH 1-2 VLA 1, L1641N MM1/3, NGC 2071 IRS 1/3, and an object in the OMC 3 region. The water masers showed significant variability in intensity and velocity with time scales of a month or shorter. Four methanol emission sources were detected, and those in the OMC 2 FIR 3/4 and L1641N MM1/3 regions are probably masers. The methanol emission from the other two sources in the NGC 2071 IRS 1-3 and V380 Ori NE regions are probably thermal. For the water masers, the number of detections per protostar in the survey region is about 2%, which suggests that the water masers of low-mass protostars are rarely detectable. The methanol class I maser of low-mass protostars is an even rarer phenomenon, with a detection rate much smaller than 1%.

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1.1.2 gamma + d -> gamma + d

Cited by 13 publications

References 1 publication

HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1

HAWC+/SOFIA Multiwavelength Polarimetric Observations of OMC-1

Submillimeter Array High-Angular Resolution Observations of the Monoceros R2 Star-Forming Cluster

Water and Methanol Maser Survey of Protostars in the Orion Molecular Cloud Complex

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