A Near-Infrared Survey of the Taurus Molecular Cloud: Near-Infrared Luminosity Function

Itoh, Yoichi; Tamura, Motohide; Gatley, I.

doi:10.1086/310154

Cited by 30 publications

(31 citation statements)

References 19 publications

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“…Thus, d(logλF λ )/d(logλ) > 0 between 1 and 10 μm, which is consistent with the classification of VLA 8A as a Class I source (e.g., Hartmann 1998). Regarding the near-infrared colors of the 2MASS sources associated with IRS 1 and VLA 8A, derived from 2MASS photometry (see Table 13), we found that both sources fall inside the area corresponding to YSOs of Class 0/I (e.g., Itoh et al 1996;Ojha et al 2004;Matsuyanagi et al 2006). Finally, VLA 8B, which is also associated with dense gas tracers, shows no infrared emission at all.…”

Section: Discussionsupporting

confidence: 86%

“…We estimated the infrared excess from the (J − H) vs. (H − J) diagram (see Table 13). The near-infrared colors derived are characteristic of main sequence stars, giants, supergiants, Class III sources, or Class II sources with small infrared excess (Itoh et al 1996;Matsuyanagi et al 2006). In addition, this source has an optical counterpart seen in the DSS2 image.…”

Section: Starless Candidates: Mm2 and The Southern Cloudmentioning

confidence: 99%

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Low-mass protostars and dense cores in different evolutionary stages in IRAS 00213+6530

Busquet¹,

Palau

Estalella³

et al. 2009

A&A

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Aims. The aim of this paper is to study with high angular resolution a dense core associated with a low-luminosity IRAS source, IRAS 00213+6530, in order to investigate whether low mass star formation is taking place in isolation. Methods. We carried out observations at 1.2 mm with the IRAM 30 m telescope, and VLA observations in the continuum mode at 6 cm, 3.6 cm, 1.3 cm and 7 mm, together with H 2 O maser and NH 3 lines toward IRAS 00213+6530. Additionally, we observed the CCS J N = 2 1 -1 0 transition, and H 2 O maser emission using the NASA 70 m antenna at Robledo de Chavela, Spain. We studied the nature of the centimeter and millimeter emission of the young stellar objects (YSOs) found in the region, and the physical properties of the dense gas and dust emission. Results. The centimeter and millimeter continuum emission, together with the near infrared data from 2MASS allowed us to identify three YSOs, IRS 1, VLA 8A, and VLA 8B, with different radio and infrared properties, and which seem to be in different evolutionary stages. IRS 1, detected only in the infrared, is in the more advanced stage. On the other hand, VLA 8A, bright at centimeter and millimeter wavelengths, coincides with a near infrared 2MASS source, whereas VLA 8B has no infrared emission associated with it and is in the earliest evolutionary stage. The overall structure of the NH 3 emission consists of three clouds. Two of these, MM1 and MM2, are associated with dust emission at millimeter wavelengths, while the southern cloud is only detected in NH 3 . The YSOs are embedded in MM1, where we found evidence of line broadening and temperature enhancements. On the other hand, the southern cloud and MM2 appear to be quiescent and starless. Concerning the 1.2 mm dust emission, we modeled the radial intensity profile of MM1. The model fits the data reasonably well, but it underestimates the intensity at small projected distances from the 1.2 mm peak, probably due to the presence of multiple YSOs embedded in the dusty envelope. There is a strong differentiation in the relative NH 3 abundance with low values of ∼2 × 10 −8 toward MM1, which harbors the YSOs, and high values, up to 10 −6 , toward the southern cloud and MM2, suggesting that these clouds could be in a young evolutionary stage. Conclusions. IRAS 00213+6530 harbors a multiple system of low-mass protostars, indicating that star formation in this cloud is taking place in groups or clusters, rather than in isolation. The low-mass YSOs found in IRAS 00213+6530 are in different evolutionary stages, suggesting that star formation takes place in different episodes.

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Section: Discussionsupporting

confidence: 86%

Section: Starless Candidates: Mm2 and The Southern Cloudmentioning

confidence: 99%

Low-mass protostars and dense cores in different evolutionary stages in IRAS 00213+6530

Busquet¹,

Palau

Estalella³

et al. 2009

A&A

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“…The multiplicative constant 1.75 in equations (1) and (2) is based on the observed reddening law (see x 3); these equations define the range of colors over which normal stars may be dereddened onto intrinsic color lines (Itoh et al 1996), as illustrated in Figure 2a. Discrimination against normal stars with little or no reddening is provided by equation (3), which effectively excludes those with visual extinctions A V < 3 mag.…”

Section: Massmentioning

confidence: 99%

A Catalog of Background Stars Reddened by Dust in the Taurus Dark Clouds

Shenoy¹,

Whittet²,

Ives³

et al. 2008

ASTROPHYS J SUPPL S

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Normal field stars located behind dense clouds are a valuable resource in interstellar astrophysics, as they provide continua in which to study phenomena such as gas-phase and solid-state absorption features, interstellar extinction, and polarization. This paper reports the results of a search for highly reddened stars behind the Taurus Dark Cloud complex. We use the Two Micron All Sky Survey (2MASS) Point Source Catalog to survey a $50 deg 2 area of the cloud to a limiting magnitude of K s ¼ 10:0. Photometry in the 1.2Y2.2 m passbands from 2MASS is combined with photometry at longer infrared wavelengths (3.6 Y12 m) from the Spitzer Space Telescope and the Infrared Astronomical Satellite to provide effective discrimination between reddened field stars and young stellar objects (YSOs) embedded in the cloud. Our final catalog contains 248 confirmed or probable background field stars, together with estimates of their total visual extinctions, which span the range 2 < A V < 29 mag. We also identify the 2MASS source J04292083+2742074 (IRAS 04262+2735) as a previously unrecognized candidate YSO, based on the presence of infrared emission greatly in excess of that predicted for a normal reddened photosphere at wavelengths >5 m.

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“…The enormous NIR dataset provided by the 2MASS (Kleinmann et al 1994) was extensively used by several authors, mainly (a) to discriminate between normal stars and stars with significant NIR emission from circumstellar material (e.g., Itoh et al 1996) and (b) to map the extinction in dense molecular clouds (Cambrésy et al 2002;Lombardi et al 2006). Dutra et al (2003) built an A K extinction map of a 10 • field towards the Galactic centre using 2MASS J and K s magnitudes.…”

Section: Introductionmentioning

confidence: 99%

A method to determine distances to molecular clouds using near-IR photometry

Maheswar

Lee²,

Bhatt

et al. 2010

A&A

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Aims. We aim to develop a method to determine distances to molecular clouds using JHK near-infrared photometry. Methods. The method is based on a technique that aids spectral classification of stars lying towards the fields containing the clouds into main sequence and giants. In this technique, the observed (J − H) and (H − K s ) colours are dereddened simultaneously using trial values of A V and a normal interstellar extinction law. The best fit of the dereddened colours to the intrinsic colours giving a minimum value of χ 2 then yields the corresponding spectral type and A V for the star. The main sequence stars, thus classified, are then utilized in an A V versus distance plot to bracket the cloud distances.Results. We applied the method to four clouds, L1517, Chamaeleon I, Lupus 3 and NGC 7023 and estimated their distances as 167 ± 30, 151 ± 28, 157 ± 29 and 408 ± 76 pc respectively, which are in good agreement with the previous distance estimations available in the literature.

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A Near-Infrared Survey of the Taurus Molecular Cloud: Near-Infrared Luminosity Function

Cited by 30 publications

References 19 publications

Low-mass protostars and dense cores in different evolutionary stages in IRAS 00213+6530

Low-mass protostars and dense cores in different evolutionary stages in IRAS 00213+6530

A Catalog of Background Stars Reddened by Dust in the Taurus Dark Clouds

A method to determine distances to molecular clouds using near-IR photometry

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