Evidence for HCO(+) infall toward T Tauri?

Langevelde, H. J. van; Dishoeck, E. F. van; Blake, Geoffrey A.

doi:10.1086/187307

Cited by 34 publications

(35 citation statements)

References 16 publications

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“…Since there appear to be larger gas concentrations in barred galaxies (Sakamoto et al 1998) and bars may be more common in type 2 Seyferts (Pogge 1989), we suggest that the reservoir of gas which appears to be present in these galaxies may provide the stability necessary to hold the molecular ring coplanar to the galactic disc. Further evidence for alignment is given by the results of Maiolino et al (1997); Papadopoulos & Seaquist (1998) who attribute the excess of star-burst activity in type 2 Seyferts to the material in the obscuring torus still being funnelled down from the global scale via the 100 pc-scale ring 35 , thus suggesting that the torus may be but a dense component of the molecular ring (Shlosman et al 1990;Friedli & Martinet 1993;Shaw et al 1993;Wilson & Tsvetanov 1994;Fosbury et al 2000;Conway 1999;Dopita et al 1998;van Langevelde et al 2000). This scenario would suggest that, in general, type 1 nuclei are more evolved than their "edge-on" counterparts; a notion supported by Blandford (1990); Maiolino et al (1997); Rigopoulou et al (1997); Dopita (1998) ;Papadopoulos & Seaquist (1998) 36 .…”

Section: Discussionmentioning

confidence: 98%

Differences in the dense gas between type 1 and type 2 Seyferts

Curran

2000

Astron. Astrophys. Suppl. Ser.

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Abstract.We have used observations of the CO J = 1 → 0 transition in a sample of 20 Seyfert galaxies in order to test the result of Heckman et al. (1989), who find that type 2 Seyferts have a higher molecular gas content than type 1 Seyferts. From our observational results alone, we, when we use all of our sample (L FIR ∼ 10 10 − 10 11 L ). The results suggest that star-burst activity is most dominant in the (L FIR ∼ 10 10 L ) type 2 Seyferts, and the relative contribution of this activity to the FIR flux (compared to the AGN) may decrease with increasing L FIR .Also, in order to test whether the Seyfert classes differ in their molecular gas distributions, we have used a simple model to estimate the inclination of the sub-kpc scale molecular ring, and, upon comparison with the observed spectra, conclude that the ring is generally aligned with the galactic disc, with the largest deviations from this being exhibited by the type 1 Seyferts. With regard to the nucleus, for most of the sample, the pc-scale obscuring torus appears to be approximately (within ≈ 30• ) aligned with the molecular ring for both Seyfert classes.

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Section: Discussionmentioning

confidence: 98%

Differences in the dense gas between type 1 and type 2 Seyferts

Curran

2000

Astron. Astrophys. Suppl. Ser.

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“…1 for images at four of the epochs). This implies that extended components of the outflow powered by T Tau S (van Langevelde et al 1994;Solf & Böhm 1999) never dominate the short-wavelength radio emission and are unlikely to affect significantly our astrometry. Since T Tau S appears as a single source, it is a priori unclear whether both components (T Tau Sa and Sb) known to exist there contribute to the total observed emission or whether one of the two components strongly dominates the flux density.…”

Section: Vatory (Nrao)mentioning

confidence: 98%

Ejection of a Low-Mass Star in a Young Stellar System in Taurus

Loinard

Rodrı́guez

Rodríguez

2003

The Astrophysical Journal

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We present the analysis of high angular resolution Very Large Array radio observations, made at 11 epochs over the last 20 years, of the multiple system T Tauri. One of the sources (Sb) in the system has moved at moderate speed (5-10 km s Ϫ1) on an apparently elliptical orbit during the first 15 yr of observations, but after a close (!2 AU) encounter with the source Sa, it appears to have accelerated westward to about 20 km s Ϫ1 in the last few years. Such a dramatic orbital change most probably indicates that Sb has just suffered an ejection-which would be the first such event ever detected. Whether Sb will ultimately stay on a highly elliptical bound orbit or whether it will leave the system altogether will be known with about 5 more years of observations.

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“…T Tauri is an interesting case in which both mechanisms occur (van Langevelde et al 1994). The flux ratios between the 1−0 S(1) and 2−1 S(1) lines can help to discriminate between the two, with higher ratios favoring shock excitation (Black & Dalgarno 1976).…”

Section: Molecular Hydrogen Emission T Tauri Northwest and The Southmentioning

confidence: 99%

New circumstellar structure in the T Tauri system

Kasper

Santhakumari

Herbst

et al. 2016

A&A

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Aims. The immediate vicinity of T Tauri was observed with the new high-contrast imaging instrument SPHERE at the VLT to resolve remaining mysteries of the system, such as the putative small edge-on disk around T Tauri Sa and the assignment of the complex outflow patterns to the individual stars. Methods. We used SPHERE IRDIS narrow-band classical imaging in Paβ, Brγ, and the ν = 1−0 S(1) line of H 2 , as well as in the nearby continua to obtain high spatial resolution and high-contrast images over the near-infrared spectral range. Line maps were created by subtracting the nearby continuum. We also reanalyzed coronagraphic data taken with SPHERE's integral field spectrograph in J-and H-band with the goal of obtaining a precise extinction estimate to T Tauri Sb, and of verifying the recently reported claim of another stellar or substellar object in the system. Results. A previously unknown coiling structure is observed southwest of the stars in reflected light, which points to the vicinity of T Tauri N. We map the circumbinary emission from T Tauri S in J-and H-band scattered light for the first time, showing a morphology that differs significantly from that observed in K-band. Molecular Hydrogen emission is found southwest of the stars, near the coiling structure. We also detect the H 2 emitting region T Tauri NW. The motion of T Tauri NW with respect to T Tauri N and S between previous images and our 2014 data provides strong evidence that the southeast-northwest outflow triggering T Tauri NW is likely to be associated with T Tauri S. We also present accurate relative photometry of the stars, which confirms that T Tauri Sa is brightening again. Our analysis rules out the presence of the recently proposed companion to T Tauri N with high confidence.

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Evidence for HCO(+) infall toward T Tauri?

Cited by 34 publications

References 16 publications

Differences in the dense gas between type 1 and type 2 Seyferts

Differences in the dense gas between type 1 and type 2 Seyferts

Ejection of a Low-Mass Star in a Young Stellar System in Taurus

New circumstellar structure in the T Tauri system

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