Access to Astronomical Catalogues

← Click to display the menu
J/ApJ/644/1006           HH 529 spectroscopy                   (Blagrave+, 2006)

A photoionized Herbig-Haro object in the Orion nebula. Blagrave K.P.M., Martin P.G., Baldwin J.A. <Astrophys. J., 644, 1006-1027 (2006)> =2006ApJ...644.1006B
ADC_Keywords: H II regions ; Stars, pre-main sequence ; Spectroscopy Keywords: dust, extinction - H II regions - ISM: Herbig-Haro objects Abstract: The spectra of Herbig-Haro objects are usually characteristic of ionization and excitation in shock-heated gas, whether an internal shock in an unsteady outflow or a bow shock interface with the interstellar medium. We examine the easternmost shock the leading optically visible shock of a Herbig-Haro outflow (HH 529) seen projected on the face of the Orion Nebula, using deep optical echelle spectroscopy, showing that the spectrum of this gas is consistent with photoionization by theta1 Ori C. By modeling the emission lines, we determine a gas-phase abundance of Fe that is consistent with the depleted (relative to solar) abundance found in the Orion nebula-evidence for the presence of dust in the nebula and therefore in the Herbig-Haro outflow. The spectrum also allows for the calculation of temperature fluctuations, t2, in the nebula and the shock. These fluctuations have been used to explain discrepancies between abundances obtained from recombination lines versus those obtained from collisionally excited lines, although to date there has not been a robust theory for how such large fluctuations (t2>0.02) can be. Description: Spectra were obtained using the echelle spectrograph on the 4m Blanco telescope at the Cerro Tololo Inter-American Observatorycovering the spectral range from the near-UV (3500Å) to the near-IR (7500Å). Three sets of red and blue spectra were obtained on two dates in 1997 and 1998. Objects: ----------------------------------------- RA (2000) DE Designation(s) ----------------------------------------- 05 35.3 -05 23 HH 529 = HH 529 ----------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 111 443 Summary of double Gaussian fits to observed echelle spectra
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 F8.3 0.1nm ID ? Wavelength identification (1) 10 A1 --- f_ID [ns] nebular or shock component 12- 19 A8 --- Ion Ion identification 21 A1 --- f_S/N [?] A low S/N (2.6<S/N<5.2) flag 23- 30 F8.3 0.1nm Wave Observed wavelength of line peak (3) 32- 36 F5.1 km/s Vel ? Line velocity 38- 40 F3.1 km/s e_Vel ? Uncertainty in Vel 42- 45 F4.1 km/s FWHM Line Full-Width at Half-Maximum (4) 47- 50 F4.1 km/s e_FWHM Uncertainty in FWHM 52- 59 F8.4 10-16W/m2/arcsec2 Icorr Reddening-corrected surface brightness (5) 61- 66 F6.4 10-16W/m2/arcsec2 e_Icorr Uncertainty in Icorr (5) 68- 72 F5.1 --- S/N Signal-to-Noise (6) 74- 79 F6.4 --- Ratio ? Shock-to-nebula surface brightness ratio (Is/In) (7) 81- 86 F6.4 --- e_Ratio ? Uncertainty in Ratio 88-111 A24 --- Notes Additional notes (8)
Note (1): Wavelength of line, in air. Wavelengths are from the Atomic Line List v2.04 (http://www.pa.uky.edu/~peter/atomic/, maintained by P.A.M. van Hoof), except O II from Blagrave & Martin (2004ApJ...610..813B). Note (3): Adjusted to rest frame of nebular H+ as defined by median of first six unblended H I Balmer lines. Note (4): A quoted FWHM of 28.3±0.0 is the result of a constrained double Gaussian fit. Note (5): Calculated from the best-fit Gaussian area and its 68.3% confidence interval. The red shock lines have been adjusted by a factor of 0.85 to correct for slit coverage differences between the red and blue spectra. The nebular lines are not adjusted. In units of 10-13erg/s/cm2/arcsec2. Note (6): From surface brightness and 68.3% confidence interval. Note (7): The shock-to-nebula ratio is entered within the nebula row and the shock row is left blank. Note (8): Additional notes as follows: C = constrained double Gaussian fit T = constrained triple Gaussian fit S = single Gaussian fit R = red echelle spectrum B = blue echelle spectrum avg = average of two orders
History: From electronic version of the journal
(End) Greg Schwarz [AAS], Patricia Vannier [CDS] 21-Sep-2007
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

catalogue service

© UDS/CNRS

Contact