THE<i>SPITZER</i>c2d SURVEY OF NEARBY DENSE CORES. VII. CHEMISTRY AND DYNAMICS IN L43

Chen, Jo-Hsin; Evans, Neal J.; Lee, Jeong Eun; Bourke, Tyler L.

doi:10.1088/0004-637x/705/2/1160

Cited by 15 publications

(30 citation statements)

References 75 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Eight of these are identified from their IRAC-MIPS colors. An additional Class I protostar exists in the L43 cloud in the center of this region (Chen et al 2009). Three further YSOcs are found based on red [K − 24] colors.…”

Section: Discussionmentioning

confidence: 99%

“…These were avoided by the Spitzer Gould Belt team to avoid unnecessary duplication of observations, as the two projects work to the same target sensitivities. Most of these c2d data are incorporated in this study of Oph N. The exception is L43 which is presented separately by Chen et al (2009). Ultimately, seven new areas were mapped by SGBS with IRAC and MIPS.…”

Section: Description Of Observationsmentioning

confidence: 99%

See 1 more Smart Citation

THESPITZERSURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. V. OPHIUCHUS NORTH OBSERVED WITH IRAC AND MIPS

Hatchell¹,

Terebey²,

Huard³

et al. 2012

ApJ

View full text Add to dashboard Cite

We present Spitzer IRAC (2.1 deg 2 ) and MIPS (6.5 deg 2 ) observations of star formation in the Ophiuchus North (Oph N) molecular clouds. This fragmentary cloud complex lies on the edge of the Sco-Cen OB association, several degrees to the north of the well-known ρ Oph star-forming region, at an approximate distance of 130 pc. The Oph N clouds were mapped as part of the Spitzer Gould Belt project under the working name "Scorpius." In the regions mapped, selected to encompass all the cloud with visual extinction A V > 3, 11 young stellar object (YSO) candidates are identified, 8 from IRAC/MIPS color-based selection and 3 from Two Micron All Sky Survey (2MASS) K S /MIPS colors. Adding to one source previously identified in L43, this increases the number of YSOcs identified in Oph N to 12. During the selection process, four color-based YSOcs were rejected as probable asymptotic giant branch stars and one as a known galaxy. The sources span the full range of YSOc classifications from Class 0/1 to Class III, and starless cores are also present. Twelve high extinction (A V > 10) cores are identified with a total mass of ∼100 M . These results confirm that there is little ongoing star formation in this region (instantaneous star formation efficiency <0.34%) and that the bottleneck lies in the formation of dense cores. The influence of the nearby Upper Sco OB association, including the 09V star ζ Oph, is seen in dynamical interactions and raised dust temperatures but has not enhanced levels of star formation in Oph N.

show abstract

Section: Discussionmentioning

confidence: 99%

Section: Description Of Observationsmentioning

confidence: 99%

THESPITZERSURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. V. OPHIUCHUS NORTH OBSERVED WITH IRAC AND MIPS

Hatchell¹,

Terebey²,

Huard³

et al. 2012

ApJ

View full text Add to dashboard Cite

show abstract

“…Instead the adopted model column density N max = 10 10 21 cm -2 was inferred by adjusting Ξ until the lower-density model contour positions approximately match those observed. This value of N max is a compromise between the peak value of the extinction map and the peak value of a higher-resolution observervation (Chen et al 2009). For the observed properties N bk = 1 10 21 cm -2 , N max = 10 10 21 cm -2 , R = 0.20 pc, and L = 1.6 pc, the derived model properties are r 0 = 0.067 pc, n 0 = 1.7 10 4 cm -3 , Ξ = 3.0, and a max = 4.0.…”

Section: Stps Model Of the L43 Filamentmentioning

confidence: 99%

Star-forming Filament Models

Myers

2017

ApJ

View full text Add to dashboard Cite

Abstract. New models of star-forming filamentary clouds are presented, to quantify their properties and to predict their evolution. These 2D axisymmetric models describe filaments having no core, one low-mass core, and one clusterforming core. They are based on Plummer-like cylinders and spheroids, bounded by a constant-density surface of finite extent. In contrast to 1D Plummer-like models, they have specific values of length and mass, they approximate observed column density maps, and their distributions of column density (N-pdfs) are polefree. Each model can estimate the star-forming potential of a core-filament system, by identifying the zone of gas dense enough to form low-mass stars, and by counting the number of enclosed thermal Jeans masses. This analysis suggests that the Musca Center filament may be near the start of its star-forming life, with enough dense gas to make its first ~3 protostars, while the Coronet filament is near the midpoint of its star formation, with enough dense gas to add ~ 8 protostars to its ~20 known stars. In contrast L43 appears near the end of its starforming life, since it lacks enough dense gas to add any new protostars to the 2 YSOs already known.

show abstract

“…Single-field interferometric observations of the close vicinity (< 10, 000 AU) of L43 also 2.5 ± 0.1 337.6 ± 18.9 0.5 a de Geus et al (1990). b Bolometric luminosity (Chen et al 2009). c Bolometric temperature (Chen et al 2009).…”

Section: Introductionmentioning

confidence: 99%

“…b Bolometric luminosity (Chen et al 2009). c Bolometric temperature (Chen et al 2009). d Central stellar mass (Levreault 1988).…”

Section: Introductionmentioning

confidence: 99%

The Disappearing Envelope Around the Transitional Class I Object L43

Koyamatsu¹,

Takakuwa²,

Hayashi³

et al. 2014

ApJ

View full text Add to dashboard Cite

We present SMA interferometric observations of the 12 CO (J = 2-1), 13 CO (J = 2-1), and C 18 O (J = 2-1) lines and 225 GHz continuum emission and SMT single-dish observations of C 18 O (J = 2-1) toward L43, a protostellar object in transition from Class I to II. The 225 GHz continuum emission shows a weak (∼ 23.6 mJy), compact (< 1000 AU) component associated with the central protostar. Our simulated observations show that it can be explained by dust thermal emission arising from an envelope which has a hole or a constant intensity region within a few hundred AU of the protostar. This suggests the disappearance or a lower concentration distribution of the envelope on a small scale. The 12 CO and 13 CO emission exhibit molecular outflows to the south and north. The C 18 O emission shows two molecular blobs, which correspond to the reflection nebulosity seen in near-infrared images, while there is no C 18 O emission associated with the protostar. The near-infrared features are likely due to the scattering at the positions of the blobs. The visible scattering features should result from the optical thinness of the envelope material, which is consistent with the less-concentrated distribution in the continuum emission. From single-dish observations, we found that the mass of the envelope (∼ 1.5 M ) + protostar (∼ 0.5 M ) is comparable with the virial mass of M vir = 1.0 M within 40 . This suggests that the envelope is likely gravitationally bound. We suggest that the protostellar envelope of L43 has been disappearing by consumption through accretion, at least in the close vicinity of the protostar.

show abstract

THESPITZERc2d SURVEY OF NEARBY DENSE CORES. VII. CHEMISTRY AND DYNAMICS IN L43

Cited by 15 publications

References 75 publications

THESPITZERSURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. V. OPHIUCHUS NORTH OBSERVED WITH IRAC AND MIPS

THESPITZERSURVEY OF INTERSTELLAR CLOUDS IN THE GOULD BELT. V. OPHIUCHUS NORTH OBSERVED WITH IRAC AND MIPS

Star-forming Filament Models

The Disappearing Envelope Around the Transitional Class I Object L43

Contact Info

Product

Resources

About