An optical and infrared study of the region surrounding Herbig-Haro objects 1 and 2

Strom, S. E.; Strom, K. M.; Grasdalen, G. L.; Sellgren, K.; Wolff, Sidney C.

doi:10.1086/113931

Cited by 42 publications

(45 citation statements)

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“…This orientation is consistent with the large-scale field structure of L1641 (Vrba et al 1988). Previous studies of the HH 1-2 region (Strom et al 1985; WS) suggested larger position angles and larger dispersions because their sample sizes were too small and because they included bright PMS stars in the sample.…”

Section: Magnetic Field Structuresupporting

confidence: 86%

“…However, the relevant physics is surprisingly complex (Lazarian 2007), and there are observational evidence and theoretical explanations for aligned grains in dense cloud cores (WardThompson et al 2000;Cho & Lazarian 2005). In the case of our study of the HH 1-2 field, the polarization degree P H does not show a clear sign of saturation up to H − K s ≈ 1 (Figure 7), Histogram of near-IR polarization position angles for the group B sources and the bright PMS stars (Strom et al 1985;Casali 1995). Note that a 20 • bin is used because the sample size is small.…”

Section: Magnetic Field Structurementioning

confidence: 73%

“…These studies covered larger regions than our study, but they were much shallower. Strom et al (1985) carried out I-band polarimetry and measured the polarization position angle of two sources: 157 • for the C-S star and 135 • for N 3 SK 50. Casali (1995) polarization angles are possible for three sources, while meaningful comparisons for polarization degrees are difficult due to wavelength dependence.…”

Section: Comparison With Previous Studiesmentioning

confidence: 99%

“…Therefore, a correction factor of ∼0.5 would be a reasonable value. For the HH 1-2 region, previously much attention was paid to the relation between the direction of the HH 1-2 outflow (position angle ≈148 • ) and the orientation of global magnetic fields (Strom et al 1985;WS). Our polarimetry shows that the difference between them (∼40 • ) is much larger than the 11 • dispersion of the polarization angles.…”

Section: Outflow Orientationsmentioning

confidence: 99%

“…This region contains several YSOs and outflows (Herbig 1951;Haro 1952;Warren-Smith et al 1980;Strom et al 1989;Corcoran & Ray 1995;Choi & Zhou 1997;Rodríguez et al 2000). The magnetic field structure in the HH 1-2 region has been studied based on optical polarizations of point sources (Strom et al 1985;Warren-Smith & Scarrott 1999, hereafter WS). They found that the local magnetic field is directed roughly along the axis of the HH 1-2 outflow, but the number of detectable stars was too small because of the large obscuration in this region.…”

Section: Introductionmentioning

confidence: 99%

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Magnetic Field Structure of the Hh 1-2 Region: Near-Infrared Polarimetry of Point-Like Sources

Kwon

Choi

Pak

et al. 2009

ApJ

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The HH 1-2 region in the L1641 molecular cloud was observed in the near-infrared (IR) J, H, and K s bands, and imaging polarimetry was performed. Seventy-six point-like sources were detected in all three bands. The near-IR polarizations of these sources seem to be caused mostly by the dichroic extinction. Using a color-color diagram, reddened sources with little IR excess were selected to trace the magnetic field structure of the molecular cloud. The mean polarization position angle of these sources is about 111 • , which is interpreted as the projected direction of the magnetic field in the observed region of the cloud. The distribution of the polarization angle has a dispersion of about 11 • , which is smaller than what was measured in previous studies. This small dispersion gives a rough estimate of the strength of the magnetic field to be about 130 μG and suggests that the global magnetic field in this region is quite regular and straight. In contrast, the outflows driven by young stellar objects in this region seem to have no preferred orientation. This discrepancy suggests that the magnetic field in the L1641 molecular cloud does not dictate the orientation of the protostars forming inside.

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Section: Magnetic Field Structuresupporting

confidence: 86%