Spatio-Kinematic Structure at the Base of the [Fe II] Jets From L1551 IRS 5

Details Spatio-Kinematic Structure at the Base of the [Fe II] Jets From L1551 IRS 5 Spatio-Kinematic Structure at the Base of the [Fe II] Jets From L1551 IRS 5

2009-01-14

arxiv.org/abs/0901.2105v1

Astrophys.J.694:654-663,2009

Astronomy and Astrophysics

Astrophysics

High Energy Astrophysical Phenomena

24 pages, 2 Tables, 6 Figures, Accepted by ApJ

Scientific paper

10.1088/0004-637X/694/1/654

We present observational results of the [Fe II] 1.644 um emission from the jets of L1551 IRS 5. The data sets were obtained through 13 fully sampled slits aimed at the base of the jets. These sets are used to construct a three-dimensional cube. The field of view was 5."8 X 4."2. We confirmed that the position of the knot PHK1 coincides with a stationary, point-like x-ray source within 0."3. The northern and southern jets are distinguished from each other at a point 0."6 away from their driving sources. We also confirmed that the northern jet consists of well-separated high- and low-velocity components (HVC and LVC, respectively). The HVC has a terminal velocity of ~400 km/s and shows a consistently narrow velocity width of 40 km/s. The LVC covers the velocity range from V_LSR = 0 to -240 km/s and has broad velocity widths of ~150-180 km/s. These decrease with distance from the driving sources. The spatial width of the LVC varies from 0."6-0."7 at V_LSR ~ -200 km/s to 0."8-0."9 at V_LSR ~ -30 km/s. These characteristics are well understood in terms of the two types of outflow mechanisms that are working simultaneously: one is the HVC, which is launched in a narrow, inner radial region at 0.04-0.05 AU, and the other is the LVC, which is launched in a wider, outer radial region from within 0.1-4.5 AU of the accretion disk. Part of the LVC emission could arise in the gas entrained or shocked by the HVC. We also discuss the possibility that part of the HVC gas is thermalized at PHK1 to produce the x-ray emission and LVC.

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