Water Maser Motions in W3(OH) and a Determination of Its Distance

Hachisuka, Kazuya; Brunthaler, A.; Menten, K. M.; Reid, M. J.; Imai, Hiroshi; Hagiwara, Yoshiaki; Miyoshi, Makoto; Horiuchi, S.; Sasao, Tetsuo

doi:10.1086/502962

Cited by 208 publications

(208 citation statements)

References 28 publications

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“…It is unlikely that the water and methanol masers originate at such different depths into the SFR that it would affect the distance. For example, in the SFR W3(OH), the water and methanol maser parallaxes are in good agreement (Xu et al 2006;Hachisuka et al 2006). NGC 281-W is an SFR that lies near the edge of a super bubble in the Perseus arm (Megeath et al 2003;Sato et al 2007).…”

Section: Ngc 281-wmentioning

confidence: 92%

Trigonometric parallaxes of 6.7 GHz methanol masers

Rygl

Brunthaler

Reid³

et al. 2010

A&A

Self Cite

153

131

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Aims. Emission from the 6.7 GHz methanol maser transition is very strong, is relatively stable, has small internal motions, and is observed toward numerous massive star-forming regions in the Galaxy. Our goal is to perform high-precision astrometry using this maser transition to obtain accurate distances to their host regions. −0.06 kpc for S 255. The distances and proper motions yield the full space motions of the star-forming regions hosting the masers, and we find that these regions lag circular rotation on average by ∼17 km s −1 , a value comparable to those found recently by similar studies.

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Section: Ngc 281-wmentioning

confidence: 92%

Trigonometric parallaxes of 6.7 GHz methanol masers

Rygl

Brunthaler

Reid³

et al. 2010

A&A

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153

131

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“…The W51 star-forming region, located at a distance of 5.1 kpc (Xu et al 2009) in the Sagittarius arm of our Galaxy, harbors two compact radio sources (Scott 1978) known as e1 and e2, which are associated with hot molecular cores with a rich chemistry (Zhang & Ho 1997;Zhang et al 1998;Ikeda et al 2001;Liu et al 2001;Remijan et al 2002;Demyk et al 2008;Kalenskii & Johansson 2010;Lykke et al 2015). The W3(OH) complex, located at 2.04 kpc (Hachisuka et al 2006), harbors two massive objects separated by 6″: the UC H II region W3(OH) (Wilner et al 1995) and the chemically rich W3(H 2 O) hot molecular core (Wyrowski et al 1999;Zapata et al 2011;Qin et al 2015).…”

Section: Introductionmentioning

confidence: 99%

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

Rivilla

Fontani

Beltrán

et al. 2016

ApJ

112

135

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Phosphorus is a crucial element in biochemistry, in particular the P−O bond, which is key in the formation of the backbone of deoxyribonucleic acid. So far, PO has only been detected toward the envelope of evolved stars, but never toward star-forming regions. We report the first detection of PO toward two massive star-forming regions, W51 e1/e2 and W3(OH), using data from the IRAM 30 m telescope. PN has also been detected toward the two regions. The abundance ratio PO/PN is 1.8 and 3 for W51 and W3(OH), respectively. Our chemical model indicates that the two molecules are chemically related and are formed via gas-phase ion-molecule and neutralneutral reactions during cold collapse. The molecules freeze out onto grains at the end of the collapse and desorb during the warm-up phase once the temperature reaches ∼35 K. Similar abundances of the two species are expected during a period of ∼5 × 10 4 yr at the early stages of the warm-up phase, when the temperature is in the range 35-90 K. The observed molecular abundances of 10 −10 are predicted by the model if a relatively high initial abundance of 5 × 10 −9 of depleted phosphorus is assumed.

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“…Radio observations with Very Long Baseline Interferometers ( VLBIs) provide an interesting alternative avenue, because they can deliver extremely accurate absolute astrometry (better than 0.1 mas) if proper calibration is applied. In the last few years, such observations have proven capable of measuring the trigonometric parallax of sources within a few kiloparsecs of the Sun with a precision of a few percent ( Brisken et al 2000( Brisken et al , 2002Loinard et al 2005Loinard et al , 2007Xu et al 2006;Hachisuka et al 2006;Hirota et al 2007;Sandstrom et al 2007). Because the sensitivity of VLBI experiments is limited, only compact nonthermal emitters can usually be detected.…”

Section: Introductionmentioning

confidence: 99%

VLBA Determination of the Distance to Nearby Star‐forming Regions. II. Hubble 4 and HDE 283572 in Taurus

Torres

Loinard

Mioduszewski

et al. 2007

ApJ

159

165

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The nonthermal 3.6 cm radio continuum emission from the naked T Tauri stars Hubble 4 and HDE 283572 in Taurus has been observed with the Very Long Baseline Array ( VLBA) at six epochs between 2004 September and 2005 December with a typical separation between successive observations of 3 months. Thanks to the remarkably accurate astrometry delivered by the VLBA, the trajectory described by both stars on the plane of the sky could be traced very precisely and modeled as the superposition of their trigonometric parallax and uniform proper motion. The best fits yield distances to Hubble 4 and HDE 283572 of 132:8 AE 0:5 and 128:5 AE 0:6 pc, respectively. Combining these results with the other two existing VLBI distance determinations in Taurus, we estimate the mean distance to the Taurus association to be 137 pc with a dispersion (most probably reflecting the depth of the complex) of about 20 pc.

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Water Maser Motions in W3(OH) and a Determination of Its Distance

Cited by 208 publications

References 28 publications

Trigonometric parallaxes of 6.7 GHz methanol masers

Trigonometric parallaxes of 6.7 GHz methanol masers

The First Detections of the Key Prebiotic Molecule Po in Star-Forming Regions

VLBA Determination of the Distance to Nearby Star‐forming Regions. II. Hubble 4 and HDE 283572 in Taurus

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