Table Of ContentA General Catalog of
HI Observations of Galaxies
W.K. Huchtmeier O.-G. Richter
A General Catalog of
HI Observations of Galaxies
The Reference Catalog
Springer-Science+Business Media, LLC
W.K. Huchtmeier
Max-Planck-Institut fUr Radioastronomie
0-5300 Bonn I, Federal Republic of Germany
O.-G. Richter
Space Telescope Science Institute
Baltimore, MD 21218, USA
also affiliated with the
Astrophysics Division of the
Space Science Department of
E.S.A.
With 8 Figures
Library of Congress Cataloging-in-Publication Data
Huchtmeier, W.K.
A general catalog of HI observations of galaxies: the reference
cataloglW. K. Huchtmeier, O. G. Richter.
p. cm.
Bibliography: p.
ISBN 978-1-4612-6418-7 ISBN 978-1-4419-8483-8 (eBook)
DOl 10.1007/978-1-4419-8483-8
1. Galaxies-Spectra-Catalogs. 2. Hydrogen-Spectra-Catalog.
I. Richter. O.-G. II. Title.
QB857.H83 1989
523.1' 12'0287-dc20 89-6356
Printed on acid-free paper.
© 1989 by Springer Science+Business Media New York
Originally published by Springer-Verlag New York Inc. in 1989
Softcover reprint of the hardcover I st edition 1989
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Camera-ready text provided by the authors.
9 8 7 654 3 2 I
Summary
A catalog of all published HI observations of external galaxies has been compiled.
Its construction is briefly described. It contains almost 20,000 entries for over
10,000 galaxies based on more than 570 references. Here the reference catalog is
presented. It contains the HI data basically just as they were originally published.
No numerical conversions were made and no error correction was attempted.
Contents
Summary ....................................................................................... \'
Introduction ...................................................................................
1\
I. The Compiled Data..............................................................
1\
1.1. References Included............................................................. 1\
1.2. Description of the Catalog ..................................................... \
1.3. Comments on Table I............................ ....... ............ .... ..... ... x
1.3.1. Galaxy Names..................................................................... x
1.3.2. Galaxy Coordinates................... ........................................... XI
1.3.3. Masses............ ............. ...................................................... XI
1.3.4. Codes Used ........................................................................ XI
1.3.5. Telescopes.......................................................................... XI
1.4. Auxiliary Information........................................................... XII
2. Some Bibliographic and a Few Other Statistics......................... XII
3. Concluding Remarks............................................... ...... ..... ... XII
Acknowledgments........................................................................... XIII
General References.......................................................................... XIII
Figures 1-8 ..................................................................................... xv
The Tables
Table 1 The Catalog..................................................................... I
Table 2a List of HI References, Ordered by Sequence Number ............. 287
Table 2b List of HI References, Ordered Alphabetically.. ..................... 298
Table 2c List of HI References, Ordered by Publication Year ............... 309
Table 3 References to Further HI Emission and Absorption
Observations.................................................................... 320
Table 4 Discussions of Global Galaxy Parameters from HI
Observations........................................ . ........................... 322
Table 5 Discussions of the Tully-Fisher Relation............................... 323
Table 6 Catalogs, Review Articles, Popular Articles, and
Miscellaneous HI References.............................................. 324
Table 7 Abstracts Published in Astron. 1. and BIIII. A.A.S. ................. 325
Table 8 Author Index with Number of References and Number of
Entries.................................................................... ........ 328
Table 9 Codes for and Number of Entries from Different Telescopes.... 339
Table 10 Galaxies Observed with Radio Interferometers....................... 340
Table II N umber of Entries Per Reference........................................ 349
Introduction
Following its theoretical prediction by H.C. van de certain values we find satisfactory agreement with those
Hulst (1945), the 21-cm spectral line of neutral hydrogen given by Bottinelli et al. (1982).
(HI) was first observed in March 1951 by Ewen and Pur No attempt was made in this reference catalog to con
cell (l95Ia,b), closely followed by confirmations by vert the data to a common scale. A later second version
groups in Holland (Muller and Oort, 1951) and Australia of the catalog will contain corrected, edited, and aver
«(f. van de Hulst, 1951). Soon its potential for galactic aged data with just one data entry per galaxy. As much
astronomy was exploited. The demonstration of the spi as possible, that second catalog will represent a homo
ral structure of our Galaxy was one of the widely recog geneous catalog.
nized early successes. Only after bigger radio tele
scopes were built and receiver technology advanced 1. The Compiled Data
were observations of external galaxies started. Of
course, the early observations concentrated on nearby
1.1. References Included
galaxies of large angular size like the Magellanic
Clouds, M31 and M33. The first publication of extraga The whole astronomical literature published until the
lactic HI measurements was by Kerr and Hindman middle of 1988 (and available to us) has been surveyed
(1953). The first HI absorption measurement, against for 21-cm line data of extragalactic objects. Every
galactic sources, was reported shortly thereafter by Ha attempt has been made to include all additional
gen and McClain (1954). references that appeared in print during the remainder
In recent years the number of accurate HI measure of 1988. Some more recent publications were included
ments of external galaxies has increased rapidly, nota when they were readily available to us. More than 900
bly due to the work of Fisher and Tully (1981). Until references in total were found. They are listed in Tables
now the multitude of these data has been widely spread 2-7.
over many different publications by different authors. In Tables 2a-c, the references actually used in the
Furthermore, some data have been presented in jour catalog (viz. Table I) are listed. While Table 2a is or
nals or books which may not be available everywhere. dered by the reference number used in Table I, Table
Some data never reached the formal publication level 2b is ordered alphabetically by authors, and Table 2c is
but may have been contained in unpublished theses. ordered chronologically. All these references give data
Clearly, all this complicates any statistical study. from 21-cm emission measurements. In general, 21-cm
The first larger data collection, published by Botti absorption data cannot be used directly to determine
nelli et al. (1982), contained exclusively those refer global properties of galaxies. References to such data
ences (until early 1980) which gave plots of global pro are listed in Table 3 together with various other emis
files. Unfortunately, it thereby neglects a large number sion references. Table 4 lists further references not
of high-quality observations. Additionally, no upper given previously which discuss global galaxian parame
limits for HI emission were cataloged. In order to rem ters on the basis of HI observations. Discussions of the
edy this situation we have compiled the present catalog, Tully-Fisher relation (Tully and Fisher, 1977) are listed
which was pre-released a few years ago (Huchtmeier in Table 5. Catalogs, review articles, and miscellaneous
et al., 1983). Some earlier references provided a global articles about HI data that have come to our attention
profile but no numerical information (e.g., Roberts, are listed in Table 6. For the sake of completeness we
1978). In those cases we have measured (graphically) have listed in Table 7 the abstracts of papers which
the profiles. For these (almost by necessity) rather un- (usually) later appeared as formal papers. Occasionally,
x
more than one reference presented the same basic data not yet contain any assumptions made by the
or discussed various aspects of them. These have been authors about linewidth and statistical uncer
combined to form a single number entry in the reference tainty;
lists.
• the radial velocity (in kill s·,) in column 10. If
The reader should note that no completeness is
specified by the authors, the reference frame is
claimed for Tables 4-6. Those reference lists are pro
coded (see below) in column 9. If no radial
vided just as an added convenience to the user of this
velocity was known and no HI detection was
catalog. Also note that references that appeared already
obtained by the authors, we list the range in
in Tables 2 or 3 are not listed again in the later Tables.
radial velocity searched for emission in columns
In Table 8 we have included an alphabetical index of
9-11 (if specified in the reference);
all authors that appear in Tables 2-7 for easy reference.
This listing will be especially useful during a search for • the error of the radial velocity (also in kill .\. . ,) in
inadvertently omitted references. column II:
1.2. Description of the Catalog • the HI line width ~I')() measured at 501/r of the
peak intensity in column 12, and
Our reference catalog is presented in Table I. It
contains-where given by the authors-the following • the HI line width ~I'\ at another (coded, see
below) level in column 13, typically at either
data:
25% or 20% of the peak flux (again in kill s·,).
• the object name in column I: The code appears in column 14;
• the most accurate known equatorial coordinates • the distance D used by the authors (in Mpc) in
(see below) in columns 2 and 3 (epoch 1950); column 15;
• the morphological type (internally coded in a • the optical dimensions a and h (in arcmin) used
crude I-byte code based on the system of the by the authors in columns 16 and 17. In rare
RC2') in column 4; cases (e.g., HI clouds) the HI size is listed;
• the inclination i (in degrees) used by the authors • the maximum rotational velocity V"UlX (in km s")
in column 5. In the rare cases where it was in column 18, and
obvious that the authors used 900-i this was
changed accordingly. In our definition i = 0° • the dynamical position angle p.a. (in degrees) in
column 19, both derived principally from HI
denotes face-on orientation;
synthesis observations;
• the HI mass (or an upper limit to it) in one of
• the number of the reference from where these
several formats in column 7. Listed are either
data were taken (see Table 2a) in column 20;
- the integrated flux I (= I S·dv) (in Jy·kms"),
• a code for the radio telescope used (cf. Table 9),
- the reduced HI mass FII (in 106 MO/Mp(2), and
denoted F, or
• an asterisk indicating that some graphical
- the derived total HI mass Mill (in 109 MO), representation of the observations (e.g., a
denoted M, or profile) and/or a photograph of this object IS
given in the reference, both in column 21.
- the logarithm of the total HI mass, denoted L.
Occasionally, only an upper limit for the peak 1.3. Comments on Table 1
flux S"UlX (denoted S) is given (in mJy). The
codes l, F, M, L, or S are given in column 6; 1. 3 .1. Ga aIxyN a mes
• the error of the quantity in column 7 appears in
Often one galaxy entered our catalog more than once
column 8. In several instances the achieved
under several different names . We attempted to retain
noise level for non-detections is given here.
S",/\ only the most "common" one. However, in some cases
For upper limits this is, in fact, the preferred
the identifications remain uncertain or ambiguous.
datum to be included in our catalog since it does
These are marked by a question mark or a colon fol
'Second Reference Catalog of Bright Galaxies (de Vaucouleurs et al., lowing the name. Most objects named "Anonymous"
1976) by the authors have been searched for in the standard
xi
galaxy catalogs, viz. the UGC2, the CGCG3, the ESO/ publication of upper limits to the HI flux without men
Uppsala catalog (Lauberts, 1982), or the MCG4 (in tioning the optical radial velocity or the observed range
order of preference). Eventually, those galaxies were of radial velocities. Such data are nevertheless included
renamed. Individual (proper) names of single galaxies for the sake of completeness. They have not been
were not used. The Small Magellanic Cloud marked specifically because the lack of such additional
(SMC = ESO 29-G 2 I) is identified as NGC 292. information is readily apparent.
1.3.2. Galaxy Coordinates 1.3.4. Codes Used
Different authors sometimes used different coordinates The radial velocities given in the catalog (Table I,
to observe the same galaxy. We give only the most column 10) are preceded by a code number indicating
accurate coordinates known to us taken either directly their reference frame as follows:
o
from the used reference, from one of the standard
Vo
galaxy catalogs, or from one or more of the following 1 VO (RC2) HI radial velocity.
references: Clements (1981), Dressel and Condon 2 VLG (RSA')
(1976), Foltz etal. (1980), Gallouet and Heidmann (1971) 3 VLSR
or Gallouet et al. (1973, 1975), Joshi and Kandalian 5 Vo
(1981), Kojoian et al. (1978, 1981a,b,c, 1982), Peterson 6 VO (RC2) optical radial velocity.
(1973), Santagata et al. (l987a,b), Vettolani et al. 7 VLG (RSA)
(1986), and Wilson and Meurs (1978). Sub-arcsecond 8
VLSR
accuracies could not be retained due to format
Usually, authors who used LSR velocities did not
limitations. In general, small differences in the observed
specify the actual reference frame. In all cases the stan
positions are not critical because the beam widths were
dard LSR is assumed.
much larger than the positional deviations. Some ref
The second linewidth given is (in virtually all cases)
erences-mostly those presenting synthesis observa
followed by a one-digit code indicating the level at
tion-give the position of the galaxy's dynamical center
which it has been measured:
derived either directly or via modelling from the
I. 2 0%
velocity field. For consistency throughout the whole
3 50% of average flux (used only by some Arecibo
catalog we have not used those, but rather have
observers)
retained the optical coordinates.
4, 6 20% of peak flux
5, 7 25% of peak flux
1.3.3. Masses
8 Rectangle model (used only by some Nan<;ay
Total masses M were included in the pre-release of this observers)
T
catalog (Huchtmeier et al., 1983) whenever available. 9 Triangle model
Occasionally they were the only item indicating the HI
The second code for the same level is used (because
linewidth or the maximum rotation velocity. Never
of internal format limitations) to identify linewidths
theless, (partially pressured by the revised format
larger than 999 km S~I; in those cases one must add 1000
requirements) we have chosen here to drop the total
km S~I to the printed value (applies to "" 5 entries). If no
masses since they are derived in a variety of different
code is given, then the level was not specified by the
ways from more basic data which are actually listed.
authors.
Unfortunately, some authors have given insufficient
information to retrieve the basic opserved data. The 1.3.5. Telescopes
most common example is the publication of an HI mass
without specifying a distance either directly or implic The one-letter codes for the different telescopes are
itly via quotation of the Hubble constant and the radial given in Table 9. Since the two 21-cm feeds in
velocity reference frame used. Another example is the Arecib~ommonly referred to as the "flat" feed and
the "circular" feed-produce quite different telescope
'Uppsala General Catalogue of Galaxies (Nilson, 1973, 1974) beam widths and, hence, different corrections for
resolution, we use both lower- and upper-case letters
lCatalogue of Galaxies and Clusters of Galaxies (Zwicky et al., for proper identification. Not always is the actually
1961-1968) used feed given. In those cases we use upper-case. As
'Morphological Catalogue of Galaxies (Vorontsov-Veljaminov et al.,
'A ReI'ised Shapley-Ames Catalog (!f' Bright Galaxies (Sandage and
1962-1974)
Tammann. 1981)
xii
can be seen from Table 9, the use of the Arecibo and holder is still M 101 (NGC 5457) with currently 31
the (former) NRAO 300-ft telescopes as redshift entries.
measurement machines ("z-machines") has led to a Another interesting statistic is the number of HI ref
total fraction of about 70% of all entries in this catalog. erences published per year. This is shown in Fig. 4. As
In general, data obtained with synthesis telescopes suming about 2-3 years time lag between conduct of ob
provide much more detail than single-dish observations. servations and actual appearance in print, one may
For the reader's convenience we list in Table 10 all gal conclude from Fig. 4. that extragalactic HI research be
axies that were observed with one of those instruments. came a really "hot" topic only around 1975. This
This list should be particularly useful for studies of HI roughly coincides with the advent of a new generation
surface density distributions and rotation curves. of low-noise 21-cm receivers at the major radio tele
scopes. From the beginning of 1954 until 1969 on aver
1.4. Auxiliary Information age only 2.5 references with extragalactic HI data were
published per year. From 1970 until 1976 the pace accel
Some other information given by the authors could not erated and this figure climbed to about 17. Since 1977 an
be included in Table 1. Nevertheless, it is sometimes average of about 33 references per year have appeared.
essential in order to make proper use of the data given The frequency distribution of the number of entries
in the catalog. Usually, those data did not fit into the provided into Table I per reference is shown in Fig. 5.
format for the main catalog. Therefore, they are Just about 50% of all references contribute only one or
currently stored separately. Among such information two entries to the catalog. While references with just
are the following items: one or two entries are "over-abundant", the overall dis
tribution is fairly flat and drops off only for references
• a flag showing the availability of coordinates
with more than about 130 entries. Nevertheless, those
directly from the HI reference,
latter references contribute more than 60% of all entries
• the Hubble constant Ho adopted by the authors, in Table 1. In this context it is also instructive to look
at the average (mean and median) number of entries per
• a flag indicating if the fluxes given were cor
reference as a function of time. Figure 6 shows the cor
rected for beam broadening or not,
responding curves. It is apparent that early observa
• the number of entries a reference contributes to tions of single galaxies were published as individual pa
Table I, and pers, whereas today researchers can conduct entire
surveys in the same amount of telescope time.
• the number of galaxies it contributes.
A final statistic we were curious about was the num
Clearly, the second and third items above are often ber of references and entries that individual authors
important for the recovery of originally measured data. contributed to the catalog. Those two frequency distri
Most of the other items are needed internally for proper butions are shown in Figs. 7 and 8.
management of the catalog. Table 11 gives the number
of entries from the different references. The other items
3. Concluding Remarks
are not printed out here but are available upon special
request.
We have presented a complete reference catalog of ex
tragalactic HI observations. The completeness of the
2. Some Bibliographic and a Few Other
catalog is estimated to be better than 95% for references
Statistics and better than 99.5% for data entries. Through two
successive proofreadings we are able to place a conser
The catalog presented in Table I contains 19,976 entries vative upper limit on the error rate in Table I of no more
for 10,308 galaxies. The actual distribution of all these than one faulty item per about 350 data lines. This
galaxies in galactic coordinates is shown in Fig. I. In should limit the total number of errors to less than about
Fig. 2 their distribution in declination is shown. Table 100. [Usually, errors or misprints in original references
11 lists the number of entries from all references (see will have propagated into our catalog.]
above). The distribution of the number of entries per The authors intend to update this catalog periodi
galaxy is shown in Fig. 3. Of course, the majority of cally. We sincerely hope that any researcher producing
all galaxies (i.e .• = 60%) have been observed just once. data that should be referenced and/or included in this
There are, on the other hand, quite a few well studied catalog will send their data to us (a) as early as possible,
galaxies with more than 10 entries each. The record and (b) preferably in computer readable form. Natu-
xiii
rally, this will ease the updating process considerably. Thanks are due to many authors who provided data in
We will gladly acknowledge the receipt of any reprints advance of publication, especially J.R. Fisher. In more
of papers to be referenced in this catalog. In order to recent years, a number of authors were kind enough to
improve the catalog as much as possible we invite inter transmit their data in computer readable form. Fortu
ested readers nately, this eliminates typing and the need for proof
reading in exchange for usually simple re-formatting.
• to point out obvious omissions from Tables 2, 3,
Here we like to thank Drs. M. Bicay, J.R. Fisher, R.
and 7,
Giovanelli, M.P. Haynes, B.M. Lewis, S.E. Schneider,
• to help completing Tables 4, 5, and 6, W.T. Sullivan III, R.B. Tully, and A. Wootten. Drs.
W.D. Pence, M.M. Phillips, W.T. Sullivan III, A.G.
• to identify typing errors or other corrections to
Turtle, and R.B. Tully kindly communicated heretofore
listed and/or originally published results,
unpublished HI observations in computer readable
• to complement the collected data with currently form. L. Dressel made her large collection of accurate
missing data items (see remarks in section coordinates for UGC galaxies available on tape.
2.3.3), We would also like to thank all those people who
made constructive comments on the form and content
• to notify us of not widely available references to of this catalog, most notably F.J. Kerr, M.S. Roberts,
be included (e.g., data currently only available and W.T. Sullivan III.
in theses, yearly reports, etc.),
• to send us data for already well-known galaxies General References
which were obtained as a secondary calibration
Bottinelli, L., Gouguenheim, L., and Paturel, G.: 1982,
or system performance check. Those data will
Astron.Astrophys.Suppl.Ser. 47, 171
ease the task of comparing flux scales. They will
Clements, E.D.: 1981, M.N.R.A.S. 197,829
receive an individual reference code (citation) in
deYaucouleurs, G., deYaucouleurs, A., and Corwin
our catalog;
Jr., H.G.: 1976, Second Reference Catalogue of
• to communicate high-quality optical data, espe Bright Galaxies, Univ. of Texas Press, Austin (RC2)
cially optical redshifts for (yet) undetected gal Dressel, L.L., and Condon, J.J.: 1976, Astrophys.
axies and total blue magnitudes in the BT system J.Suppl. 31, 187
of the RC2. Ewen, H.I., and Purcell, E.M.: 1951a, Astron.J. 56, 125
Ewen, H.I., and Purcell, E.M.: 1951b, Nature 168, 356
Fisher, J.R., and Tully, R.B.: 1981, Astrophys.J.Suppl.
Acknowledgments
47, 139
In 1974 Paris Pismis initiated a collection of data on in Foltz, C.B., Peterson, B.M., and Boroson, T.A.: 1980,
ternal velocity information of extragalactic systems. In Astron.J. 85, 1328
1976 the project was announced at a session of the Gallouet, L., and Heidmann, N.: 1971, Astron.Astro
"Working group on internal motions in galaxies" (sub phys.Suppl.Ser. 3,325
group of l.A. U. commission 28) at Grenoble. The col Gallouet, L., Heidmann, N., and Dampierre, F.: 1973,
lection of the data was performed as a background job Astron.Astrophys.Suppl.Ser. 12, 89
and the ideas about its presentation changed substan Gallouet, L., Heidmann, N., and Dampierre, F.: 1975,
tially until 1981. Astron .Astrophys .Suppl.Ser. 19, I
The early stages of this work were financially sup Hagen, J.P., and McClain, E.F.: 1954, Astrophys.J.
ported by the Deutsche Forschungsgemeinschaft (DFG) 120,368
under grant Hu 234/3. The project would have been im Huchtmeier, W.K., Richter, O.-G., Bohnenstengel, H.
possible without the support of the Hamburger Stern D., and Hauschildt, M.: 1983, ESO Scientific Preprint
warte and the help of several staff members, most nota no. 250
bly H.-D. Bohnenstengel and M. Hauschildt. We would Joshi, M.N., and Kandalian, R.A.: 1981, Bull.Astr.Soc.
like to thank the European Southern Observatory which India 9, 24
made it possible to publish the pre-release version of Kerr, F.J., and Hindman, J.Y.: 1953, Astron.J. 58, 212
this catalog in printed form. Special thanks go to Dave Kojoian, G., Elliot, R., and Tovmassian, H.M.: 1978,
Davis (S.T.Sc.I.), whose help during the final assembly Astron.J. 83, 1545
of the catalog into its present form was instrumental for Kojoian, G., Elliot, R., and Tovmassian. H.M.: 1981a,
the success of the project. Astron.J. 86, 811
