VLBA Determination of the Distance to Nearby Star‐forming Regions. I. The Distance to T Tauri with 0.4% Accuracy

Loinard, Laurent; Torres, Rosa M.; Mioduszewski, Amy J.; Rodrı́guez, Luis F.; González-Lópezlira, Rosa A.; Lachaume, R.; Vázquez, Virgilio; Gonzalez, Erandy

doi:10.1086/522493

Cited by 174 publications

(187 citation statements)

References 26 publications

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“…For example, the Perseus distance is in excellent agreement with recent multi-epoch VLBI maser observations of the YSO SVS 13 in NGC 1333 (Hirota et al 2008), which provide d Perseus = (235 ± 18) pc. Similarly, the Taurus distance is in excellent agreement with a VLBI determination, d Taurus = (147.6±0.6) pc (Loinard et al 2007). Finally, we note that the accuracy and reliability of the distances based on the density of foreground stars suggests that we can use this technique for clouds for which no VLBI distance is available (such as the California cloud) or possible (for example because of the lack of maser sources or of the large distance of the clouds).…”

Section: Notessupporting

confidence: 82%

“…There have also been extensive dust extinction studies done of the Taurus dark clouds (Straizys & Meistas 1980;Meistas & Straizys 1981;Cernicharo & Bachiller 1984;Cernicharo & Guelin 1987;Cernicharo et al 1985;Cambrésy 1999;Dobashi et al 2005) using either star counts or color-excesses. The current best estimate of the distance to the Taurus complex, using VLBI, is (147.6 ± 0.6) pc (Loinard et al 2007). These authors also found that the thickness of the complex is comparable to its extent, or about 20 pc.…”

Section: Introductionmentioning

confidence: 95%

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2MASS wide field extinction maps

Lombardi

Lada

Alves

2010

A&A

129

126

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We present a near-infrared extinction map of a large region in the sky (∼3500 deg 2 ) in the general directions of Taurus, Perseus, and Aries. The map has been obtained using robust and optimal methods to map dust column density at near-infrared wavelengths (Nicer, described in Lombardi & Alves 2001, A&A, 377, 1023 and Nicest, described in Lombardi 2009 toward ∼23 million stars from the Two Micron All Sky Survey (2MASS) point source catalog. We measure extinction as low as A K = 0.04 mag with a 1-σ significance, and a resolution of 2.5 arcmin in our map. A 250 deg 2 section of our map encompasses the Taurus, Perseus, and California molecular cloud complexes. We determine the distances of the clouds by comparing the observed density of foreground stars with the prediction of galactic models, and we obtain results that are in excellent agreement with recent VLBI parallax measurements. We characterize the large-scale structure of the map and find a ∼25 • × 15 • region close to the galactic plane (l ∼ 135 • , b ∼ −14 • ) with small extinction (A K < 0.04 mag); we name this region the Perseus-Andromeda hole. We find that over the region that encompasses the Taurus, Perseus, and California clouds the column density measurements below A K < 0.2 mag are perfectly described by a log-normal distribution, and that a significant deviation is observed at larger extinction values. If turbulence models are invoked to justify the log-normal distribution, the observed departure could be interpreted as the result of the effect of gravity that acts on the cores of the clouds. Finally, we investigate the cloud structure function, and show that significant deviations from the results predicted by turbulent models are observed in at least one cloud.

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Section: Notessupporting

confidence: 82%

Section: Introductionmentioning

confidence: 95%

2MASS wide field extinction maps

Lombardi

Lada

Alves

2010

A&A

129

126

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“…Many VLBAdetected YSOs belong to tight multiple systems (Ortiz-León et al 2016). In some systems a close companion could cause differences of measured proper motions between the VLA and the VLBA, since the former will measure the total motion of the system and the latter could be dominated by an orbital motion component (e.g., Loinard et al 2007). More recent VLBA observations of GMRG by Kounkel et al (2016a) obtained different values for the proper motions than those reported by Menten et al (2007) suggesting that the motion of the source is not uniform, perhaps due to a close companion.…”

Section: Resultsmentioning

confidence: 99%

Radio Measurements of the Stellar Proper Motions in the Core of the Orion Nebula Cluster

Dzib

Loinard

Rodrı́guez

et al. 2017

ApJ

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Using multi-epoch Very Large Array observations, covering a time baseline of 29.1 years, we have measured the proper motions of 88 young stars with compact radio emission in the core of the Orion Nebula Cluster (ONC) and the neighboring BN/KL region. Our work increases the number of young stars with measured proper motion at radio frequencies by a factor of 2.5 and enables us to perform a better statistical analysis of the kinematics of the region than was previously possible. 1.27 0.15 mas yr −1 . We looked for organized movements of these stars but found no clear indication of radial expansion/contraction or rotation. The remaining nine stars in our sample show peculiar proper motions that differ from the mean proper motions of the ONC by more than 3σ. One of these stars, V1326 Ori, could have been expelled from the Orion Trapezium 7000 years ago. Two could be related to the multi-stellar disintegration in the BN/KL region, in addition to the previously known sources BN, I and n. The others either have high uncertainties (so their anomalous proper motions are not firmly established) or could be foreground objects.

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“…The equations governing the parallax displacements can be found, for example, in Brisken et al (2002) and Loinard et al (2007). The additional displacements were added to the data before performing the fit, and are not included in Table 6.…”

Section: Uncertainties In the Position Of Ls 5039mentioning

confidence: 99%

On the origin of LS 5039 and PSR J1825−1446

Moldón

Ribó

Paredes

et al. 2012

A&A

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Context. The gamma-ray binary LS 5039 and the isolated pulsar PSR J1825−1446 were proposed to have been formed in the supernova remnant (SNR) G016.8−01.1. Aims. We aim to obtain the Galactic trajectory of LS 5039 and PSR J1825−1446 to find their origin in the Galaxy, and in particular to check their association with SNR G016.8−01.1 to restrict their age. Methods. By means of radio and optical observations we obtained the proper motion and the space velocity of the sources. Results. The proper motion of PSR J1825−1446 corresponds to a transverse space velocity of 690 km s −1 at a distance of 5 kpc. Its Galactic velocity at different distances is not compatible with the expected Galactic rotation. The velocity and characteristic age of PSR J1825−1446 make it incompatible with SNR G016.8−01.1. There are no clear OB associations or SNRs crossing the past trajectory of PSR J1825−1446. We estimate the age of the pulsar to be 80-245 kyr, which is compatible with its characteristic age. The proper motion of LS 5039 is μ α cos δ = 7.09 and μ δ = −8.82 mas yr −1 . The association of LS 5039 with SNR G016.8−01.1 is unlikely, although we cannot discard it. The system would have had to be formed in the association Ser OB2 (at 2.0 kpc) if the age of the system is 1.0-1.2 Myr, or in the association Sct OB3 (distance 1.5-2 kpc) for an age of 0.1-0.2 Myr. If the system were not formed close to Ser OB2, the pseudo-synchronization of the orbit would be unlikely. Conclusions. PSR J1825−1446 is a high-velocity isolated pulsar ejected from the Galaxy. The distance to LS 5039, which needs to be constrained by future astrometric missions such as Gaia, is a key parameter for restricting its origin and age.

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VLBA Determination of the Distance to Nearby Star‐forming Regions. I. The Distance to T Tauri with 0.4% Accuracy

Cited by 174 publications

References 26 publications

2MASS wide field extinction maps

2MASS wide field extinction maps

Radio Measurements of the Stellar Proper Motions in the Core of the Orion Nebula Cluster

On the origin of LS 5039 and PSR J1825−1446

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