The optical spectrum of L1551 IRS 5

Mundt, R.; Stocke, John T.; Strom, S. E.; Strom, K. M.; Anderson, E.

doi:10.1086/184554

Cited by 69 publications

(30 citation statements)

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“…Adams, Lada, & Shu (1987) identified it as a protostellar (Class I) source with an estimated infall rate for its envelope of ∼ 10 −5 M ⊙ yr −1 . The near-infrared spectrum exhibits first-overtone absorption in CO, suggesting that IRS 5 is an FU Ori object (Carr, Harvey, & Lester 1987), consistent with an analysis of the optical spectrum observed in scattered light (Mundt et al 1985 andStocke et al 1988). Given the wide variety of observational constraints available, L1551 IRS 5 is clearly an ideal system for investigating the circumstellar environment that surrounds protostars and to understand its implications for the general process of star formation.…”

Section: Introductionsupporting

confidence: 81%

A Comprehensive Study of the L1551 IRS 5 Binary System

Osorio

D’Alessio

Muzerolle

et al. 2003

ApJ

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We model the Class I source L1551 IRS 5, adopting a flattened infalling envelope surrounding a binary disk system and a circumbinary disk. With our composite model, we calculate self-consistently the spectral energy distribution of each component of the L1551 IRS 5 system, using additional constraints from recent observations by ISO, the water ice feature from observations with SpeX, the SCUBA extended spatial brightness distribution at sub-mm wavelengths, and the VLA spatial intensity distributions at 7 mm of the binary disks. We analyze the sensitivity of our results to the various parameters involved. Our results show that a flattened envelope collapse model is required to explain simultaneously the large scale fluxes and the water ice and silicate features. On the other hand, we find that the circumstellar disks are optically thick in the millimeter range and are inclined so that their outer parts hide the emission along the line of sight from their inner parts. We also find that these disks have lower mass accretion rates than the infall rate of the envelope.Comment: 38 pages, 13 figures. To appear in ApJ (v586 April 1, 2003 issue

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Section: Introductionsupporting

confidence: 81%

A Comprehensive Study of the L1551 IRS 5 Binary System

Osorio

D’Alessio

Muzerolle

et al. 2003

ApJ

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“…The strong absorption bands and the absorption feature at ∼6500 Å could indicate that the spectral type is similar to an M 2 giant. The absorption feature at ∼6500 Å arises from a blend of Fe I, Ca I and Ba II lines and is also seen in FU Orionis type stars (Mundt et al 1985). The spectrum looks very similar to that of PP 13N as shown in Fig.…”

Section: Spectra Of Be Stars and Some Probable Pms Starssupporting

confidence: 54%

NGC 146: a young open cluster with a Herbig Be star and intermediate mass pre-main sequence stars

Subramaniam¹,

Sahu²,

Sagar³

et al. 2005

A&A

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Abstract. We present UBV CCD photometry and low-resolution spectra of stars in the field of the young open cluster NGC 146. UBV photometry of 434 stars were used to estimate the E(B − V) reddening of 0.55 ± 0.04 mag and BV photometry of 976 stars were used to estimate a distance modulus of (m − M) 0 = 12.7 ± 0.2 mag, corresponding to a distance of 3470pc. We estimated 10-16 Myr as the turn-off age for the upper main sequence of the cluster using isochrones and synthetic colour magnitude diagrams. We identified two B type stars with H α in emission and located on the MS using slit-less spectra. A higher resolution spectrum of the brighter Be star indicated the presence of a number of emission lines, with some lines showing the signature of gas infall. This star was found to be located in the region of Herbig Ae/Be stars in the (J − H) vs. (H − K) colour-colour diagram. Thus, we identify this star as a Herbig Be star. On the other hand, 54 stars were found to show near infrared excess, of which 17 were found to be located in the region of Herbig Ae/Be stars and 18 stars were found to be located in the region of Be stars in the NIR colour-colour diagram. Thus NGC 146 is a young cluster with a large number of intermediate mass pre-main sequence stars. The turn-on age of the cluster is found to be ∼3 Myr. Though NGC 146 shows an older turn off, the bulk of stars in this cluster seems to belong to the younger population of 3 Myr.

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“…A number of luminous stars in star-forming regions have been found that possess some or all of the characteristics of FUors, but for which no eruptions were witnessed. Objects in this category include Z CMa (e.g., Hartmann et al 1989), L1551 IRS5 (e.g., Mundt et al 1985;Carr et al 1987), and BBW 76 (e.g., Reipurth et al 2002). A number of more deeply embedded objects show the deep broad CO band head absorption characteristic of FUors, including RNO 1B/C and Parsamian 21 (Staude & Neckel 1991Kenyon et al 1993), V883 Ori (Strom & Strom 1993;Reipurth & Aspin 1997), Haro 5a IRS, HH 354 IRS, and HH 381 IRS ( Reipurth & Aspin 1997), PP 13S (Sandell & Aspin 1998), and AR6A/6B (Aspin & Reipurth 2003).…”

Section: Introductionmentioning

confidence: 99%

V733 Cep (Persson's Star): A New FU Orionis Object in Cepheus

et al. 2007

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Persson recently found that a faint star had appeared in a cloud in Cepheus. A CCD image shows a R $ 17:3 nebulous star, now known as V733 Cep, located in the L1216 = Cep F cloud at the apex of a cavity in the cloud. Infrared photometry indicates a modest infrared excess. Optical spectroscopy shows a well-defined Li i k6707 line, and blueshifted absorption troughs at the H and Na i D lines extending to at least 200 km s À1 , indicative of a massive fast wind. An infrared 1-4 m spectrum of V733 Cep shows the presence of strong water vapor features, and is almost identical to a similar IR spectrum of FU Ori that is reddened by A V ¼ 8 mag. Assuming an intrinsic energy distribution similar to that of FU Ori, V733 Cep has a luminosity of about 135 L at the assumed distance of 800 pc. The star was detected by the Midcourse Space Experiment satellite at 8.3 m, but not by IRAS. Nor is it detected at 850 m, indicating that while the star possesses circumstellar material it is not surrounded by a significant cool envelope. A 12 CO(3-2) map shows what appears to be a small molecular outflow along the same axis as the cavity seen in optical images. There is evidence for a limited amount of other low-and medium-mass star formation in the Cep F cloud. The totality of the evidence strongly indicates that V733 Cep is a new FU Ori-type object that must have erupted sometime between 1953 and 1984.

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The optical spectrum of L1551 IRS 5

Cited by 69 publications

References 0 publications

A Comprehensive Study of the L1551 IRS 5 Binary System

A Comprehensive Study of the L1551 IRS 5 Binary System

NGC 146: a young open cluster with a Herbig Be star and intermediate mass pre-main sequence stars

V733 Cep (Persson's Star): A New FU Orionis Object in Cepheus

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