VLBA Determination of the Distance to Nearby Star-forming Regions. II. Hubble 4 and HDE 283572 in Taurus

By R. Torres, L. Loinard, A. Mioduszewski, Luis F. Rodriguez. 2007

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The nonthermal 3.6 cm radio continuum emission from the naked T Tauri stars Hubble 4 and HDE 283572 in Taurus has been observed with the Very Long Baseline Array (VLBA) at six epochs between 2004 September and 2005 December with a typical separation between successive observations of 3 months. Thanks to the remarkably accurate astrometry delivered by the VLBA, the trajectory described by both stars on the plane of the sky could be traced very precisely and modeled as the superposition of their trigonometric parallax and uniform proper motion. The best fits yield distances to Hubble 4 and HDE 283572 of 132.8 ± 0.5 and 128.5 ± 0.6 pc, respectively. Combining these results with the other two existing VLBI distance determinations in Taurus, we estimate the mean distance to the Taurus association to be 137 pc with a dispersion (most probably reflecting the depth of the complex) of about 20 pc.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/35cc2cd390e07e973e0b5fe7185a9561449b1a6a

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Citations in the corpus

Microarcsecond Radio Astrometry (2013, unknown): “The Taurus molecular cloud has been well studied and parallaxes for five YSOs have been reported from VLBA observations in a series of papers (Loinard et al. 2005, 2007; Torres et al. 2007, 2009, 2012).”
AN INFRARED/X-RAY SURVEY FOR NEW MEMBERS OF THE TAURUS STAR-FORMING REGION (2009, methodology): “…the extinctions with J-band photometry from the Point Source Catalog of the Two-Micron AllSky Survey (2MASS; Skrutskie et al. 2006), a distance of 140 pc (Wichmann et al. 1998; Loinard et al. 2005, 2007; Torres et al. 2007, 2009), and the bolometric corrections used by Luhman (2004a, 2007).”
Fundamental Parameters of the Milky Way Galaxy Based on VLBI Astrometry (2012, unknown): “…2012, (27) Sakai et al. 2012, (28) Sanna et al. 2009, (29) Sanna et al. 2012, (30) Sato et al. 2008, (31) Sato et al. 2010a, (32) Sato et al. 2010b, (33) Shiozaki et al. 2011, (34) Torres et al. 2007, (35) Torres et al. 2009, (36) Xu et al. 2006, (37) Xu et al. 2009, (38) Xu et al. 2011, (39)…”
The Disk Around CoKu Tauri/4: Circumbinary, Not Transitional (2008, background): “An uncertainty in distance due to the depth of Taurus (e.g. Torres et al. 2007) can not reconcile this discrepancy, as both RD determined from radiative transfer modeling and the minimum RD determined by dynamical considerations both increase linearly with the distance estimate.”
Probing the evolution of molecular cloud structure: From quiescence to birth (2009, unknown): “…45011 9.0 1.2 1.7 0.59 > 100 Cepheus A 73013 3.5 1.5 1.6 0.47 > 100 California 45014 11 1.4 0.7 0.51 tens a References: (1) Lombardi et al. (2008b) (2) Torres et al. (2007) (3) Straižys et al. (1996) (4) Knude & Hog (1998) (5) Casey et al.(1998) (6) Kun (1998) (7) Lombardi et al. (2006) (8)…”
Precision Timing of PSR J0437–4715: An Accurate Pulsar Distance, a High Pulsar Mass, and a Limit on the Variation of Newton’s Gravitational Constant (2008, methodology): “Following Damour & Taylor (1991) this can be translated into a limit on the time derivative of Newton’s gravitational constant (given are 95% confidence levels): Ġ G ¼ 1 2 Ṗb Pb excess ¼ ( 5 18) ; 10 12 yr 1: ð4Þ This limit is of the same order as those previously derived from pulsar timing (see x”
BANYAN. VII. A NEW POPULATION OF YOUNG SUBSTELLAR CANDIDATE MEMBERS OF NEARBY MOVING GROUPS FROM THE BASS SURVEY (2015, background): “A distance larger than 82 pc can be excluded at a 99% confidence level, which is incompatible with membership to TAU (140± 20 pc; Torres et al. 2007) unless it is an unresolved multiple with at least 3 individual equal-luminosity components.”
MAPPING THE SHORES OF THE BROWN DWARF DESERT. II. MULTIPLE STAR FORMATION IN TAURUS–AURIGA (2011, background): “…and from binary orbit fitting (Boden et al. 2007) suggest that there might be a distance gradient of 165-125 pc in the east-west direction, especially given the consistent distances of neighboring stars V773 Tau and Hubble 4 (136.2±3.7 pc versus 132.5±0.6 pc; Boden et al. 2007; Torres et al. 2007).”
VLBA DETERMINATION OF THE DISTANCE TO NEARBY STAR-FORMING REGIONS. III. HP TAU/G2 AND THE THREE-DIMENSIONAL STRUCTURE OF TAURUS (2009, methodology): “Introduction Several recent observations (e.g. Loinard et al. 2005, 2007, 2008; Torres et al. 2007; Menten et al. 2007; Xu et al. 2006) have demonstrated that multi-epoch VLBI observations can be used to measure the trigonometric parallax of nearby young starsto better than a few percent.”
A Preliminary VLBA Distance to the Core of Ophiuchus, with an Accuracy of 4% (2008, methodology): “Since the density of compact quasars known around Ophiuchus at the time of our observations was insufficient, we could not apply the multi-source calibration described in Torres et al. (2007).”
THE TAURUS SPITZER SURVEY: NEW CANDIDATE TAURUS MEMBERS SELECTED USING SENSITIVE MID-INFRARED PHOTOMETRY (2009, background): “At just 137 pc (with a depth of ∼ 20 pc; Torres et al. 2007, 2009), the Taurus star-forming region is one of the closest large cloud complexes with hundreds of low-mass stars, ongoing star formation, and objects ranging in age up to ∼5 Myr.”
The Bar and Spiral Structure Legacy (BeSSeL) Survey: Mapping the Milky Way with VLBI Astrometry† (2011, background): “Most radio stars are relatively weak, and the sensitivity of current instruments limits the detection to sources within a few hundred parsec (e.g. Loinard et al. 2007; Menten et al. 2007; Torres et al. 2007).”