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J/ApJ/478/603       L1448 & L 1455 new Herbig-Haro flows (Bally+ 1997)
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New Herbig-Haro flows in L1448 and L1455
       Bally J., Devine D., Alten V., Sutherland R.S.
      <Astrophys. J. 478, 603 (1997)>
      =1997ApJ...478..603B      (SIMBAD/NED BibCode)
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ADC_Keywords: Stars, pre-main sequence ; Radial velocities
Keywords: ISM: individual (L1448) - ISM: jets and outflows -
          stars: pre-main-sequence

Abstract:
    We present a deep narrowband H{alpha} and [S II] optical survey of a
    roughly 1deg^2^ region containing L1448 and L1455 in the southwestern
    region of the Perseus molecular cloud. We report the detection of 13
    new groups of Herbig-Haro (HH) objects in this region. The L1448 core
    contains eight groups of Herbig-Haro objects (HH 193, HH 194, HH 195,
    HH 196, HH 197, HH 267, HH 268, and HH 277). Many of the new HH
    objects near L1448 have orientations similar to the L1448C molecular
    jet and L1448 IRS3 outflow. All four known infrared sources in L1448
    power Herbig-Haro objects. L1448 IRS 1 is the likely source of HH 194,
    HH 195E, and possibly HH 268. L1448 IRS 2 drives HH 195, and L1448 IRS
    3 may power HH 196 and possibly HH 193. HH 267 and HH 277 lie close to
    the axes of the IRS 2 and IRS 3 flows and may also be powered by one
    of these sources. Finally, the class 0 source L1448C powers HH 197.
    The L1455 core contains five new groups of HH objects (HH 278, HH 279,
    HH 280, HH 317, and HH 318). L1455 IRS 1 and L1455 IRS 2 are likely to
    power HH objects, but a unique association between each IRAS source
    and a specific HH object is difficult to make. Both clouds contain
    some HH objects whose driving sources cannot be conclusively
    identified. Most of the new HH objects are located near the cloud
    edges while some are in the interclump medium (ICM) more than 1pc from
    the nearest cloud core or known young stellar object. These
    observations provide further evidence that HH flows can extend far
    beyond the cloud cores containing their sources, and in some cases
    extend over greater distances than associated high-velocity
    millimeter-wavelength CO emission. Herbig-Haro objects associated with
    the terminal working surfaces of outflows located in the ICM can be
    used to probe the nature of the interclump gas in molecular clouds.
    The large number of HH objects found in relatively inactive star
    forming regions such as L1448 and L1455 indicates that shock heating
    and acceleration by protostellar outflows plays an important role in
    determining the ionization state and energetics of the ICM that
    surrounds low-mass star forming regions.

File Summary:
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  FileName        Lrecl  Records   Explanations
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ReadMe             80        .   This file
table1             76       24   L1448 HH objects
table2             74       11   L1455 HH objects
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Byte-by-byte Description of file: table1 table2
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   Bytes Format Units      Label     Explanations
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   1-  6  A6    ---        HH        HH name
       7  A1    ---      m_HH        [ABCDE] Multiplicity index on HH
       9  I1    h          RAh       Right ascension (1950)
  11- 12  I2    min        RAm       Right ascension (1950)
  14- 17  F4.1  s          RAs       Right ascension (1950) (1)
  20- 21  I2    deg        DEd       Declination (1950)
  23- 24  I2    arcmin     DEm       Declination (1950)
  26- 27  I2    arcsec     DEs       Declination (1950) (1)
  30- 33  F4.1 10-18W/m2   SHa       H{alpha} flux (2)
  36- 39  F4.1 10-18W/m2   S[SII]    ? [S II] flux (2)
  42- 45  I4   arcsec+2    Area      Area
  48- 50  I3    km/s       RV        ? Radial velocity of the HH object
  53- 55  I3    km/s       DV        ? Line width of the HH object
  58- 77  A20   ---        Source    Source name
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Note (1): Coordinates are accurate to within a few arcseconds.
Note (2): Line fluxes are in units of 10^-15ergs/cm^2/s and were calibrated
           by observations of the standard Feige 34. Fluxes were determined
           by integrating the emission (summing the counts in each pixel) over
           the apparent extent of the HH object, then subtracting the background
           integrated over a nearby region of the same size that was free
           from HH emission.
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History: Prepared via OCR at CDS.
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(End)                          James Marcout,  Patricia Bauer [CDS]  03-Oct-1997