/pub/Catalogs/Herbig-Haro,
which contains, in addition to a readme file, the three files:
catalogue.tex, notes.tex, references.tex.
Reference to this catalogue should be done as follows:
Reipurth, B.: 1994, A general catalogue of Herbig-Haro objects,
electronically published via anon. ftp to ftp.hq.eso.org, directory
/pub/Catalogs/Herbig-Haro.
In the days when discoveries of HH objects were rare and only few people worked in the field it was possible to assign consecutive HH numbers to the objects as they became known. This has long since become impossible, and lacking some sort of coordinating facility, newly discovered HH objects have been given a great variety of names (e.g. S140/HH3, GGD 34, N2264 HH 14-4, RNO 40E, WSB 47, Re 4 head, GN20.18.3/HH, Th 28, HHG33.3+0.2).
About two years ago I was approached by Dr. M.-C. Lortet of the IAU Nomenclature Committee, who asked me if something could be done to bring order to this wild growing subject. After some hesitation I embarked upon a survey of the entire literature on Herbig-Haro flows with the aim to produce a complete catalogue of all known HH objects, and the result is presented here. The philosophy is closer to that of Herbig's 1974 catalogue than to that of the von Hippel, Burnell, Williams 1988 catalogue. The present catalogue contains three parts. First, a table listing for each object an HH number, any previous designations, a position, identification of a suspected driving source, the name of the general region of the object, and a distance estimate. Second, a note section where each object is briefly described and extensive and as complete as possible references are given to the literature. Third, a section with references, where also the title is listed, to help give a first idea about the content of a paper. The catalogue is thus less a source of information, and more a tool to find information.
All known HH objects accepted as such now have an HH number, in continuation of the already existing HH numbers assigned by Herbig and others. In most cases this is a great improvement over previous designations. In a few cases well known and beloved names have been sacrificed, with regret, for the sake of the larger vision of having once and for all a single nomenclature system that gives a complete description of an increasingly important class of astrophysical objects. When an object had to be renamed, a special effort was made to find a number that, whenever possible, was somehow related to the previous name. Thus RNO 40 and 43 are now HH 240 and 243, Th 28 is HH 228, M16-HH1 is HH 216, the M42 objects HH 1-10 are HH 201 - 210, GGD34 is HH 234, etc. Hopefully any transition difficulties will be shortlived.
A statistical analysis of the entire material presented here is presently being carried out, and will be published separately.
Another technique, pioneered by Solf, is to place a long slit on a young star at a variety of position angles. Very short HH flows, that would be difficult to see in a direct image where the brightness of the star could swamp it, will appear clearly after elimination of the stellar continuum. I have used the guideline that such flows that extend more than several arcseconds from a star, and which could thus in principle be studied morphologically using proper coronagraphic techniques, are included in the catalogue. Stars with HH emission lines but no appreciable extent have not been included.
With the advent of infrared imaging detectors, many HH objects have
been found to emit significantly in H
and [FeII] with roughly
similar morphologies at optical and infrared wavelengths. A number of
molecular hydrogen objects have been detected in embedded molecular
outflows with no optical counterparts. While it seems probable that
these objects differ from ordinary HH objects only in the amount of
extinction along the line-of-sight, much work on the infrared
properties of HH flows remains to be done before it can be justified
to expand the definition of HH objects to include all objects only
detected in the infrared. However, this rule can be relaxed where
there is additionally strong morphological support for classification
as an HH flow. Thus, in this catalogue two objects, HH 121 and HH 211,
have been included which are well collimated bipolar
flows, located in regions of star formation and up to now only
detected at infrared wavelengths.
In recent years an increasing number of shocked regions have been found in association with evolved stars. Kinematically and morphologically these objects do not appear to differ much from Herbig-Haro objects, but spectroscopically they are rather different because the shocks occur in highly processed material. From the point of view of hydrodynamics and shock physics these objects are undoubtedly as interesting as HH flows and supernova remnants and other supersonic flows. However, the most important aspect of the Herbig-Haro phenomenon is arguably the unique insights which it has provided into the processes that lead to the formation of stars. For this reason it was felt that HH flows should remain strictly as a star formation phenomenon, as it was originally defined by Herbig and Haro. Thus, this catalogue does not contain any objects which arise from evolved stars.
A limitation of the present catalogue is the absence of images of the various HH objects. It is planned that one of the next versions will be made available for MOSAIC and will include images.
While a major effort has been invested in making the references to work on individual objects as complete as possible, it is inevitable that some important references could be missing. Certainly not all papers mentioning a given object should be listed, and an estimate of relevance has been applied to all papers. For a little known object even a single poor observation can be helpful, but it could be irrelevant for very well studied regions like L1551. So no universal rule of inclusion can be made. If you feel that a useful reference is missing, please send an e-mail to me at reipurth@eso.org.