Bow shocks in a newly discovered maser source in IRAS 20231+3440

Ogbodo, C. S.; Burns, Ross; Handa, Toshihiro; Omodaká, Toshihiro; Nakagawa, Akiharu; Nagayama, Tomonori; Honma, Mareki; Chibueze, James O.; Ubachukwu, A. A.; Eze, R. N. C.

doi:10.1093/mnras/stx1154

Cited by 5 publications

(2 citation statements)

References 30 publications

(57 reference statements)

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“…The strongest water masers occur on the western side of the apex at a projected distance of ≈ r 0 from both the apex and the axis of the bow shock. The total width of the bow shock traced by CM2-W1 (∼500 au) is similar to the size scale of maser arcs that are perpendicular to the outflow direction as seen in VLBI observations of more distant massive star formation regions like W49N (Gwinn 1994), and somewhat larger than the maser arcs recently resolved in AFGL 5142 (Burns et al 2016) and IRAS 20231+3440 (Ogbodo et al 2017). Thus, these maser features appear to be a common result of the impact of high-velocity jets from massive protostars.…”

Section: The Water Maser Bow Shocksupporting

confidence: 76%

The Extraordinary Outburst in the Massive Protostellar System NGC 6334I-MM1: Flaring of the Water Masers in a North–South Bipolar Outflow Driven by MM1B

Brogan

Hunter

Cyganowski

et al. 2018

ApJ

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We compare multi-epoch sub-arcsecond VLA imaging of the 22 GHz water masers toward the massive protocluster NGC 6334I observed before and after the recent outburst of MM1B in (sub)millimeter continuum. Since the outburst, the water maser emission toward MM1 has substantially weakened. Simultaneously, the strong water masers associated with the synchrotron continuum point source CM2 have flared by a mean factor of 6.5 (to 4.2 kJy) with highly-blueshifted features (up to 70 km s −1 from LSR) becoming more prominent. The strongest flaring water masers reside 3000 au north of MM1B and form a remarkable bow shock pattern whose vertex coincides with CM2 and tail points back to MM1B. Excited OH masers trace a secondary bow shock located ∼120 au downstream. ALMA images of CS (6-5) reveal a highly-collimated north-south structure encompassing the flaring masers to the north and the non-flaring masers to the south seen in projection toward the MM3-UCHII region. Proper motions of the southern water masers over 5.3 years indicate a bulk projected motion of 117 km s −1 southward from MM1B with a dynamical time of 170 yr. We conclude that CM2, the water masers, and many of the excited OH masers trace the interaction of the high velocity bipolar outflow from MM1B with ambient molecular gas. The previously-excavated outflow cavity has apparently allowed the radiative energy of the current outburst to propagate freely until terminating at the northern bow shock where it strengthened the masers. Additionally, water masers have been detected toward MM7 for the first time, and a highly collimated CS (6-5) outflow has been detected toward MM4.

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Section: The Water Maser Bow Shocksupporting

confidence: 76%

The Extraordinary Outburst in the Massive Protostellar System NGC 6334I-MM1: Flaring of the Water Masers in a North–South Bipolar Outflow Driven by MM1B

Brogan

Hunter

Cyganowski

et al. 2018

ApJ

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“…The above physical properties from observations yield a momentum rate Ṗ ∼ 4 × 10 −3 M ⊙ yr −1 km s −1 for the protostellar outflow of M17 MIR. This is comparable to outflows of 10 −3 − 10 0 M ⊙ yr −1 km s −1 driven by MYSOs (Moscadelli et al 2016), and one magnitude higher than the outflow from a low-mass YSO in IRAS 20231+3440 (Ogbodo et al 2017).…”

Section: Outflow Rate and Disk Accretion Rate Of M17 Mirmentioning

confidence: 64%

M17 MIR: A massive protostar with multiple accretion Outbursts

Chen,

Sun,

Chini

et al. 2021

Preprint

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We report the discovery of a massive protostar M17 MIR embedded in a hot molecular core in M17. The multi-wavelength data during 1993 to 2019 show significant mid-IR (MIR) variations, which can be split into three stages, the decreasing phase during 1993.03 to mid 2004, the quiescent phase during mid 2004 to mid 2010, and the re-brightening phase since mid 2010 untill now. The 22 GHz H 2 O maser emission variation, together with the MIR variation, indicate an enhanced disk accretion rate onto M17 MIR during the decreasing and re-brightening phase. Radiative transfer modeling of the spectral energy distributions of M17 MIR in the 2005 (quiescent) and 2017 epoch (accretion outburst) constrains the basic stellar parameters of M17 MIR, which is an intermediate-mass protostar (M * ∼ 5.4 M ⊙ ) with Ṁacc ∼ 1.1 × 10 −5 M ⊙ yr −1 in the 2005 epoch and Ṁacc ∼ 1.7 × 10 −3 M ⊙ yr −1 in the 2017 epoch. The enhanced Ṁacc during outburst induces the luminosity outburst ∆L ≈ 7600 L ⊙ .In the accretion outburst, a larger stellar radius is required to produce Ṁacc consistent with the value estimated from the kinematics of H 2 O masers. M17 MIR shows two accretion outbursts (∆t ∼ 9 − 20 yr) with outburst magnitudes of about 2 mag, separated by a 6 yr quiescent phase. The fraction time of accretion ourbusrt is 83% over 26 yr. The accretion rate in outburst is variable with amplitude much lower than the contrast between quiescent and ourbusrt phase. The extreme youth of M17 MIR suggests that minor accretion bursts are frequent at the earliest stages of massive star formation.

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The First VERA Astrometry Catalog

Hirota¹,

Nagayama²,

Honma³

et al. 2020

Publications of the Astronomical Society of Japan

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We present the first astrometry catalog from the Japanese VLBI (very long baseline interferometer) project VERA (VLBI Exploration of Radio Astrometry). We have compiled all the astrometry results from VERA, providing accurate trigonometric-annual-parallax and proper-motion measurements. In total, 99 maser sources are listed in the VERA catalog. Among them, 21 maser sources are newly reported, while the rest of the 78 sources are referred to in previously published results or those in preparation for forthcoming papers. The accuracy in the VERA astrometry is revisited and compared with that from the other VLBI astrometry projects such as BeSSeL (The Bar and Spiral Structure Legacy) Survey and GOBELINS (the Gould’s Belt Distances Survey) with the VLBA (Very Long Baseline Array). We have confirmed that most of the astrometry results are consistent with each other, and the largest error sources are due to source structure of the maser features and their rapid variation, along with the systematic calibration errors and different analysis methods. Combined with the BeSSeL results, we estimate the up-to-date fundamental Galactic parameters of $R_{0}=7.92\pm 0.16_{\rm {stat.}}\pm 0.3_{\rm {sys.}}\:$kpc and $\Omega _{\odot }=30.17\pm 0.27_{\rm {stat.}}\pm 0.3_{\rm {sys.}}\:$km$\:$s$^{-1}\:$kpc$^{-1}$, where $R_{0}$ and $\Omega _{\odot }$ are the distance from the Sun to the Galactic center and the Sun’s angular velocity of the Galactic circular rotation, respectively.

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Bow shocks in a newly discovered maser source in IRAS 20231+3440

Cited by 5 publications

References 30 publications

The Extraordinary Outburst in the Massive Protostellar System NGC 6334I-MM1: Flaring of the Water Masers in a North–South Bipolar Outflow Driven by MM1B

The Extraordinary Outburst in the Massive Protostellar System NGC 6334I-MM1: Flaring of the Water Masers in a North–South Bipolar Outflow Driven by MM1B

M17 MIR: A massive protostar with multiple accretion Outbursts

The First VERA Astrometry Catalog

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