Astrometry of H$_{2}$ O Masers in Nearby Star-Forming Regions with VERA. IV. L 1448 C

Hirota, Tomoya; Honma, Mareki; Imai, Hiroshi; Sunada, Kazuyoshi; Ueno, Yuji; Kobayashi, Hideyuki; Kawaguchi, Noriyuki

doi:10.1093/pasj/63.1.1

Cited by 90 publications

(87 citation statements)

References 45 publications

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“…The L1448-mm/IRS3 region L1448 is a dense globule located in the nearby complex of dark clouds in Perseus (Bachiller & Cernicharo 1986), at a distance of 235 pc (Hirota et al 2011). Associated with the globule are three IRAS sources, named IRS 1, 2, and 3; IRS3 being the most prominent source at infrared wavelengths (Bachiller & Cernicharo 1986).…”

Section: The Sourcesmentioning

confidence: 99%

Warm gas in protostellar outflows

Gómez-Ruiz

Wyrowski

Leurini

et al. 2013

A&A

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Context. Observations of CO rotational transitions in the 0.3−0.4 millimeter range, now possible from exceptional sites on the ground, provide the opportunity of studying the warm component of molecular outflows in star-forming regions. Aims. This study aims to characterize the role of the warm gas in high-velocity and collimated outflows from Class 0 low-mass protostars. Methods. We used the CHAMP + heterodyne array on the APEX telescope to map the CO (6-5) and CO (7-6) emission in the wellknown Class 0 outflows L1448-mm and HH211-mm. We complement these data with 13 CO (6-5) observations and also with previous low-J CO observations. Results. The CO (6-5) and (7-6) emission was detected to be tracing the outflow lobes. In L1448, extremely high-velocity (EHV) emission was detected in both transitions. In HH211, high-velocity CO (6-5) emission was detected to be tracing the regions close to the central object, but it was also found close to the bow-shock regions seen in the mid-IR. A large velocity gradient code applied to these and the complementary low-J CO data revealed the high-velocity components to be dense (>10 5 cm −3 ) and warm (T > 200 K) gas, in agreement with previous observations of shock tracers such as SiO. Conclusions. The high-velocity emission of these mid-J CO transitions are very good tracers of the inner highly excited part of outflows, which possibly is molecular material related to the underlying jet. In addition, these transitions are also strong at the bowshock positions, which make them a good tool for probing these environments.

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Section: The Sourcesmentioning

confidence: 99%

Warm gas in protostellar outflows

Gómez-Ruiz

Wyrowski

Leurini

et al. 2013

A&A

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“…HBC 340 forms a visual pair with the M5-type pre-main-sequence star HBC 341, lying ∼5 1 to the northeast. Adopting the distance of NGC 1333 derived by Hirota et al (2007Hirota et al ( , 2011, ∼235±18 pc, the angular separation of HBC 340 and HBC 341 implies a projected physical distance of ∼1200 au, consistent with a widely separated, pre-main-sequence binary (Mathieu 1994).…”

Section: Introductionmentioning

confidence: 66%

“…Assuming the distance derived by Hirota et al (2007Hirota et al ( , 2011, this angle implies a projected physical separation of ∼235 au. From aperture photometry of the source, we determine =  m 20.33 0.03…”

Section: Optical Imaging Of the Reflection Nebulamentioning

confidence: 83%

“…We estimate the extinction corrected, R C magnitude by assuming A V ∼8.0 mag and using the normal extinction law (R=3.1, Mathis 1990) to derivẽ A 6.0 R mag. Adopting a distance, d, of 235 pc (Hirota et al 2007(Hirota et al , 2011 and assuming the ratio of fluxes at λ6563 and λ6410 to be near unity, we calculate the accretion luminosity using the following relationship from Alcalá et al (2014): From the accretion luminosity, the mass accretion rate,Ṁ, follows from Gullbring et al (1998):…”

Section: Keck High-dispersion Spectroscopy Of Hbc 340 and Hbc 341mentioning

confidence: 99%

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Interpretation of a Variable Reflection Nebula Associated with HBC 340 and HBC 341 in NGC 1333

Dahm

Hillenbrand

2017

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We present multi-epoch, R-band imaging obtained from the Palomar Transient Factory of a small, fan-shaped reflection nebula in NGC 1333 that experiences prominent brightness fluctuations. Photometry of HBC 340 (K7e) and HBC 341 (M5e), a visual pair of late-type, young stellar objects lying near the apex of the nebula, demonstrates that while both are variable, the former has brightened by more than two magnitudes following a deep local minimum in 2014 September. Keck high-dispersion (R∼45,000-66,000), optical spectroscopy of HBC 340 suggests that the protostar is a spectroscopic binary (HBC 340Aa + HBC 340Ab). Both HBC 340 and HBC 341 exhibit strong Hα and forbidden line emission, consistent with accretion and outflow. We conclude that the brightness fluctuations in the reflection nebula represent light echos produced by varying incident radiation emanating from HBC 340. The short-term variability observed in the protostar is attributed to irregular accretion activity, while correlated, dipping behavior on a several hundred day timescale may be due to eclipse-like events caused by orbiting circumstellar material. Archival Hubble Space Telescope imaging of the region reveals a second, faint (F814W∼20.3 mag) companion to HBC 340 that lies 1 02 (∼235 au) east of the protostar. If associated, this probable substellar mass object (20-50 Jupiter masses), HBC 340B, is likely unrelated to the observed brightness variations. The sustained brightening of HBC 340 since late 2014 can be explained by an EXor-like outburst, the recovery from a long duration eclipse event caused by obscuring circumstellar dust, or by the gradual removal of extincting material from along the line of sight. Our analysis here favors one of the extinction scenarios.

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“…The Oort constant was A = 13.2 ± 6.4 km s rest (U ⊙ , V ⊙ , W ⊙ ) LSR makes a major contribution to the group velocity (21). The residual velocity is quite low: it is virtually zero along the z coordinate, while it is 4-10 km s…”

Section: Cloudsmentioning

confidence: 96%

The system of molecular clouds in the Gould Belt

Бобылев

2016

Astron. Lett.

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Abstract-Based on high-latitude molecular clouds with highly accurate distance estimates taken from the literature, we have redetermined the parameters of their spatial orientation. This system can be approximated by a 350 × 235 × 140 pc ellipsoid inclined by the angle i = 17 ± 2• to the Galactic plane with the longitude of the ascending node l Ω = 337 ± 1• . Based on the radial velocities of the clouds, we have found their group velocity relative to the Sun to be (u 0 , v 0 , w 0 ) = (10.6, 18.2, 6.8) ± (0.9, 1.7, 1.5) km s −1 . The trajectory of the center of the molecular cloud system in the past in a time interval of ∼60 Myr has been constructed. Using data on masers associated with lowmass protostars, we have calculated the space velocities of the molecular complexes in Orion, Taurus, Perseus, and Ophiuchus. Their motion in the past is shown to be not random.

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Astrometry of H$_{2}$ O Masers in Nearby Star-Forming Regions with VERA. IV. L 1448 C

Cited by 90 publications

References 45 publications

Warm gas in protostellar outflows

Warm gas in protostellar outflows

Interpretation of a Variable Reflection Nebula Associated with HBC 340 and HBC 341 in NGC 1333

The system of molecular clouds in the Gould Belt

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