| Full text | |
| Author(s): Show less - |
Ortiz-Leon, Gisela N.
[1]
;
Loinard, Laurent
[2, 3]
;
Dzib, Sergio A.
[1]
;
Galli, Phillip A. B.
[4]
;
Kounkel, Marina
[5]
;
Mioduszewski, Amy J.
[6]
;
Rodriguez, Luis F.
[3]
;
Torres, Rosa M.
[7]
;
Hartmann, Lee
[8]
;
Boden, Andrew F.
[9]
;
Evans, II, Neal J.
;
Briceno, Cesar
[10]
;
Tobin, John J.
[11, 12]
Total Authors: 13
|
| Affiliation: Show less - | [1] Max Planck Inst Radioastron, Hugel 69, D-53121 Bonn - Germany
[2] Univ Nacl Autonoma Mexico, Inst Astron, Apartado Postal 70-264, Mexico City 04510, DF - Mexico
[3] Univ Nacl Autonoma Mexico, Inst Radioastron & Astrofis, Morelia 58089, Michoacan - Mexico
[4] Univ Sao Paulo, Inst Astron Geofis & Ciencias Atmosfer, Rua Matao 1226, Sao Paulo - Brazil
[5] Western Washington Univ, Dept Phys & Astron, 516 High St, Bellingham, WA 98225 - USA
[6] Natl Radio Astron Observ, Domenici Sci Operat Ctr, 1003 Lopezville Rd, Socorro, NM 87801 - USA
[7] Univ Guadalajara, Ctr Univ Tonala, Ave Nuevo Perifer 555, Tonala 48525, Jalisco - Mexico
[8] Univ Michigan, Dept Astron, 500 Church St, Ann Arbor, MI 48105 - USA
[9] CALTECH, Div Phys Math & Astron, 1200 East Calif Blvd, Pasadena, CA 91125 - USA
[10] Evans, Neal J., II, Cerro Tololo Interamer Observ, Casilla 603, La Serena - Chile
[11] Univ Oklahoma, Homer L Dodge Dept Phys & Astron, 440 W Brooks St, Norman, OK 73019 - USA
[12] Leiden Observ, POB 9513, NL-2300 RA Leiden - Netherlands
Total Affiliations: 12
|
| Document type: | Journal article |
| Source: | ASTROPHYSICAL JOURNAL; v. 865, n. 1 SEP 20 2018. |
| Web of Science Citations: | 14 |
| Abstract | |
We derive the distance and structure of the Perseus molecular cloud by combining trigonometric parallaxes from Very Long Baseline Array (VLBA) observations, taken as part of the GOBELINS survey and Gaia Data Release 2. Based on our VLBA astrometry, we obtain a distance of 321 +/- 10 pc for IC 348. This is fully consistent with the mean distance of 320 +/- 26 measured by Gaia. The VLBA observations toward NGC 1333 are insufficient to claim a successful distance measurement to this cluster. Gaia parallaxes, on the other hand, yield a mean distance of 293 +/- 22 pc. Hence, the distance along the line of sight between the eastern and western edges of the cloud is similar to 30 pc, which is significantly smaller than previously inferred. We use Gaia proper motions and published radial velocities to derive the spatial velocities of a selected sample of stars. The average velocity vectors with respect to the LSR are ((u) over bar, (v) over bar, (w) over bar) = (-6.1 +/- 1.6, 6.8 +/- 1.1, -0.9 +/- 1.2) and (-6.4 +/- 1.0, 2.1 +/- 1.4, -2.4 +/- 1.0) km s(-1) for IC. 348 and NGC 1333, respectively. Finally, our analysis of the kinematics of the stars has shown that there is no clear evidence of expansion, contraction, or rotational motions within the clusters. (AU) | |
| FAPESP's process: | 13/04934-8 - Kinematics and Evolution of Pre-Main Sequence Stars in Nearby Star-Forming Regions |
| Grantee: | Phillip Andreas Brenner Galli |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |
| FAPESP's process: | 15/14696-2 - Complementing Gaia from the ground with the dance survey in nearby star-forming regions |
| Grantee: | Phillip Andreas Brenner Galli |
| Support Opportunities: | Scholarships abroad - Research Internship - Post-doctor |