Structures and optical IDs for 1103 B3 sources

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1989AJ.....98..419Vigotti+
Optical Identifications of B3 Radio Sources (37d<Dec<47d)

Description

This catalog contains results of a large program of optical identifications of radio sources from the Third Bologna (B3) Catalog (Ficarra et al., 1985). A homogeneous sample of 1103 radio sources, selected from the B3 catalog at 408 MHz and covering a flux density range from 2.0 to 0.1 Jy, has been mapped at 1465 MHz using the VLA at 15" resolution. Both positional and structural information have been derived and are presented here. Optical identifications have been attempted for all of the sources within the range of right ascension studied, using the Palomar Sky Survey prints, resulting in 354 proposed identifications. The RA range was restricted to exclude sky areas at low galactic latitude, because obscuration makes these unsuitable for optical identifications, and confusion makes them unsuitable for VLA snapshot-mode observations. Thus the samples were selected only from the RA intervals 23h-3h, 7h-15h. The number of rows of this table (1474) is larger than the number of sources (1103) because each radio component of multiple sources is listed as a separate line. These data were originally presented in Vigotti et al. 1989, A.J., 98, 419.
Contact: C. S. Grant, SAO; stern@cfa.harvard.edu (3/93)
Subject   Optical Identifications of B3 Radio Sources (37d<Dec<47d)
history   from Heinz Andernach's collection of catalogs (a016)
origin    submitted by M. Vigotti
date      08-Mar-1993
revised   15-Jun-1993
columns   22
rows      1474



-----Name----|--Units--|---Description-----------------------------------|
name                    Name of source (char9, example: '0739+397a')
othername               3C or 4C name of source (char5, example: '38.02')
sample                  Number of B3 sample which contained source
sample                  (int, example: 0)
ra_1950       radians   Right ascension of source in radians (B1950)
ra_1950                 (real, example: 2.006023)
dec_1950      radians   Declination of source in radians (B1950)
dec_1950                (real, example: 0.694166)
ra_1950_deg   degrees   Right ascension of source in degrees (B1950)
ra_1950_deg             (real, example: 114.936668)
dec_1950_deg  degrees   Declination of source in degrees (B1950)
dec_1950_deg            (real, example: 39.772778)
flux_flg                Flagged if flux is integrated or upper limit
flux_flg                (char1, example: '+' or '-')
s1465         mJy       Flux density at 1465 MHz in mJy (real, example: 46)
morph                   Morphological classification of source
morph                   (char4, example: 'D190' or 'R 12')
s408          Jy        Flux density at 408 MHz in Jy (real, example: 0.150)
alpha                   Spectral index between 1465 and 408 MHz
 alpha                   (real, example: -0.740)
id                      Proposed source identification
id                      (char3, example: ' G?' or ' N' or '*G')
z_flag                  Flagged '*' if redshift is from the literature
z_flag                  (char1, example: '*')
z                       Estimated or measured redshift (real, example: 0.198)
mag                     Red magnitude (real, example 16.5)
opt_ra                  Seconds of RA (B1950) for optical position
opt_ra                  (real, example: 8.250)
opt_dec                 Arcseconds of Dec (B1950) for optical position
opt_dec                 (real, example: 6.300)
delta_ra                Radio-optical RA offset (real, example: -0.1)
delta_dec               Radio-optical Dec offset (real, example: -0.8)
pos_flg                 Flag indicating which radio position was adopted
pos_flg                 (int, example: 4)
ref                     Reference code (int, example: 16)


 1.  COLUMNS name   othername  


The IAU name is given in the name column.  This was not given in the B3
Catalogue, and was obtained from the B3 position (hours, minutes, degrees,
and tenths of degrees) adding a letter (a, b, etc.) in order of right
ascension, in case of ambiguity.  Note that this designation does not
always match the new VLA position, although this happens rarely.  In the
case of physically connected multiple sources, a single name is given if
they correspond to a single source in the B3 Catalogue; however, some
sources listed separately in B3 happen to be parts of the same source
(e.g. 0050+401, 0050+403, and 0050+402B) and in this case they retain their
individual B3 names.

    The othername column gives the 4C name.  If the source is also in the
3CR Catalogue, the 3CR name is given instead.  3CR names are recognizable
by the format (integer number, or at most one decimal digit), while 4C names
are in the DD.NN format.  Identification with a 4C source is sometimes
ambiguous, as discussed in the B3 Catalogue.


 2.  COLUMN 'sample' 

     This column indicates the source parent subsample.  This number
indicates inclusion in the sample as originally selected; for example,
the physical double 0218+399(A+B) is listed as


       0218+399A    1 

       0218+399B    2


since the respective B3 flux densities are 0.36 and 0.49 Jy, and the
components were originally selected as parts of two different samples.
The VLA map showed them to be part of the same source; consequently the
total 408 MHz flux density is now listed as 0.85 Jy (s408 column) and in
any subsequent analysis the source will be considered part of sample 3,
0.8 ' S ' 1.6 Jy.
     Another example is given by the following double source 0218+402(A+B);
only one component (A) was originally included in sample 2 (although both
components are separately listed in B3) since component B did not meet the
selection criteria as given in the published paper.  See the paper for full
details.


 3.  COLUMNS 'ra_1950' 'dec_1950' 'ra_1950_deg' 'ra_1950_deg'

     These columns give the B1950 position of the source (or component) in
radians and in degrees.  When no source component was detected with the
VLA, the flux_flg column is marked with an '-' and the given position
is from B3 (Ficarra et al. 1985).

 4.  COLUMNS 'flux_flg' 's1465'

     The flux_flg column is marked with a "+" if the source (component) was
resolved, and an integrated flux density is given.  A '-' in the flux_flg
column indicates that the source component was not detected with the VLA
and the given flux is an upper limit.  For these sources, the listed
position is from B3.  The s1465 columns gives the source (or component)
flux density at 1465 MHz in mJy.


 5.  COLUMN 'morph'

 This column gives a simple morphological classification of the radio
structure, as follows:

	U   unresolved, the synthesized beam is not appreciably broadened.

	R   resolved, only one emission peak is present, but the source map
	      or 'response' is wider than the antenna beam.

	D   double source, two emission peaks are present and they appear
	      to be physically related.

	T   triple source, three peaks present and possibly related.

The morphological classification is followed by the source largest angular
size (LAS), measured in arcseconds.  U implies an (average) upper limit of
5 arcsec; R sources were given a size by measuring the largest HPBW, and
deconvolving it with the antenna beam; for D and T sources the separation
between the (outermost) components is given.


 6.  COLUMN 's408'

     This column gives the total 408 MHz flux density in Jy; generally it
is taken from B3, but for extended, strong sources it has been remeasured
integrating from the B3 map on the structure revealed by the VLA data.


 7.  COLUMN 'alpha'

     This column gives the spectral index, computed between 1465 and 408
MHz.  For multiple sources, the 1465 MHz flux densities have been added.
Alpha is defined in the sense S prop nu^(alpha).


 8.  COLUMN 'id'

 This column gives the proposed optical identification, as follows:


	G   galaxy

	B   starlike, blue object

	N   starlike object of neutral color


Note that the optical identification for multiple sources (e.g. type D or T)
is ONLY given for the FIRST listed component, and omitted for all others.

A question mark indicates an uncertain optical classification, it does
*not* necessarily indicate an uncertain identification.  An asterisk
preceeding the optical classification indicates that the identification
was accepted even if it does not meet a uniform criterion of positional
agreement (see the paper for details).  Note that this column is three
characters, with the optical identification being the second character.
Thus, to search for all galaxies, one must search for all sources like
'%G' since a percent sign is the wildcard in SQL.


 9.  COLUMNS 'z_flag' 'z' 'mag'

     For galaxies, the redshift is given in the z column.  If a spectroscopic
redshift is available in the literature, the z_flag column is marked with an
asterisk (*).  In this case the reference given in the ref column is to the
redshift measurement.  To estimate redshifts for those not available in the
literature, the image size was measured and from it the redshift was inferred,
following an established procedure for radio galaxies (Sandage 1972; Grueff
and Vigotti 1989).  The method has been recalibrated using spectroscopic
redshifts available for 33 radio galaxies in our sample.  Some of these are
available in the literature, and many were measured by Kron (1986) as an
optical followup of this program.
     For N and B objects, the red magnitude is given, except for some B
objects, whose spectroscopic redshift from the literture is given.


 10. COLUMNS 'opt_ra' 'opt_dec' 

     These columns give the seconds of right ascension and arcseconds of
declination of the optical object;  hours and minutes in RA and degrees and
arcminutes in dec. are generally given by the radio position.  This allows
the recovery of full optical positional information.
     Note that for positions near full minutes of time in R.A. or arcmin in
Dec., the RA-minute or Dec-arcmin for the optical position may be different
by one unit (e.g. in 1250+384).

 11. COLUMNS 'delta_ra' 'delta_dec' 

     These columns give the radio-minus-optical coordinates differences,
in arcsec.


 12. COLUMN 'pos_flg' 

     This column gives a single digit indicating, for multiple sources, the
radio position adopted as follows:

	1   first component
	2   second component
	3   third component
	4   unweighted average position (midpoint)
	5   weighted average position (radio centroid)


 13. COLUMN 'ref' 

     This column gives a reference code number.  For sources with a measured
redshift, only the reference for the redshift is given; for 3CR sources, the
reader is referred also to Spinrad et al. (1985).  The following references
are used:

	1   Allington-Smith, J.R., et al. 1982.

	2   Arp, H.C., et al. 1979.

	3   Baldwin, J.A., et al. 1973.

	4   Borngen, F., et al. 1970.

	5   Bozyan, E.P. 1979.

	6   Burbidge, E.M. 1970.

	7   Burbidge, E.M., et al. 1972.

	8   Cohen, A.M., et al. 1977.

	9   Colla, G., et al. 1975.

	10  Condon, J.J., et al. 1979.

	11  Davies, R.D. 1973.

	12  De Veny, J.B., et al. 1971.

	13  Edwards, T., et al. 1975.

	14  Fanti, C., et al. 1981.

	15  Fanti, R., et al. 1978.

	16  Gregory, S.A. and Burns, J.O. 1982.

	17  Johnson, K.H. 1974.

	18  Katgert-Merkelijn, J., et al. 1980.

	19  Kuhr, H.  1977.

	20  Kuhr, H.  1980.

	21  Lynds, R. and Wills, D.  1968.

	22  Maltby, P., et al. 1963.

	23  Olsen, E.T. 1970.

	24  Padrielli, L. and Conway, R.G.  1977.

	25  Peterson, B.M., et al. 1978.

	26  Porcas, R.W., et al. 1980.

	27  Richter, G.A., et al. 1974.

	28  Rudnick, L. and Adams, M.T.  1979.

	29  Rudnick, L. and Owen, F.N.  1977.

	30  De Ruiter, H.R., et al. 1977.

	31  Sandage, A.  1966.

	32  Sandage, A.  1967.

	33  Sandage, A., et al. 1976.

	34  Sargent, W.L.W.  1973.

	35  Schmidt, M. 1965.

	36  Schmidt, M. 1974.

	37  Smith, H.E. and Spinrad, H.  1980.

	38  Smith, H.E., et al.  1976.

	39  Spinrad, H.  1982.

	40  Spinrad, H. and Smith, H.E.  1973.

	41  Spinrad, H., et al. 1981.

	42  Strittmatter, P.A., et al. 1974.

	43  Ulrich, M.H.  1976.

	44  Walsh, D. and Carswell, R.F.  1982.

	45  Walsh, D., et al.  1979.

	46  Wilkinson, A., et al.  1981.

	47  Wills, B.J. and Wills, D.  1979.

	48  Wills, D. and Wills, B.J.  1976.

	49  Willson, M.A.G.  1972.

	50  Grueff, G. and Vigotti, M.  1979.

	51  Cohen, A.M., et al.  1977.

	52  Kriss, G.A. and Canizares, C.R.  1982.

	53  Walsh, D., et al.  1984.


References

Allington-Smith, J.R., Perryman, M.A.C., Longair, M.S., Gunn, J.E., and
  Westphal, J.A.  1982,  M.N.R.A.S., 201, 331.

Arp, H.C., de Ruiter, H.R., and Willis, A.G.  1979, A&A, 77, 86.

Baldwin, J.A., Burbidge, E.M., Hazard, C., Murdoch, H.S., Robinson, L.B., and
  Wampler, E.J.  1973, Ap.J., 185, 739.

Borngen, F., Bronkalla, W., and Dautcourt, G.  1970, Ap.J., 162, 337.

Bozyan, E.P.  1979, A.J., 84, 910.

Burbidge, E.M.  1970, Ap.J.Lett., 160, L33.

Burbidge, E.M., and Strittmatter, P.A.  1972, Ap.J.Lett., 174, L57.

Cohen, A.M., Porcas. R.W., Browne, I.W.A., Daintree, E.J., and Walsh, P.  1977,
  Mem.R.A.S., 84, 1.

Colla, G., Fanti, C., Fanti, R., Gioia, I., Lari, C., Lequeux, J., Lucas, R.,
  and Ulrich, M.H.  1975, A&A.Suppl., 20, 1.

Condon, J.J., Buckman, M.A., and Machalski, J.  1979, A.J., 84, 149.

Davies, R.D.  1973, M.N.R.A.S., 161, 25P.

De Ruiter, H.R., Willis, A.G., and Arp, H.  1977, A&A.Suppl., 28, 211.

De Veny, J.B., Osborn, W.H., and Janes, K.  1971, P.A.S.P., 83, 611.

Edwards, T., Kronberg, P.P., and Menard, G.  1975, A.J., 80, 1005.

Fanti, C., Fanti, R., Feretti, L., Ficarra, A., Gioia, I.M., Giovannini, G.,
  Gregorini, L., Mantovani, F., Marano, B., Padrielli, L., Parma, P., Tomassi,
  P., and Vettolani, G.  1981, A&A, 105, 200.

Fanti, R., Gioia, I., Lari, C., and Ulrich, M.H.  1978, A&A.Suppl., 34, 341.

Ficarra, A., Grueff, G., Tomassetti, G., 1985, Astron. Astrophys. Suppl.
  Ser., 59, 255.

Gregory, S.A. and Burns, J.O.  1982, Ap.J., 255, 373.

Grueff, G. and Vigotti, M.  1977, A&A, 54, 475.

Grueff, G. and Vigotti, M.  1979, A&A.Suppl., 35, 371.

Johnson, K.H.  1974, A.J., 79, 1006.

Katgert-Merkelijn, J., Lari, C., and Padrielli, L.  1980, A&A.Suppl., 40, 91.

Kriss, G.A. and Canizares, C.R.  1982, Ap.J., 261, 51.

Kuhr, H.  1977, A&A.Suppl. 29, 139.

Kuhr, H.  1980, Ph.D. thesis, University of Bonn.

Lynds, R. and Wills, D.  1968, Ap.J.Lett., 153, L23.

Maltby, P., Matthews, T.A., and Moffett, A.T.  1963, Ap.J., 137, 153..

Olsen, E.T.  1970, A.J., 75, 764.

Padrielli, L. and Conway, R.G.  1977, A&A.Suppl., 27, 171.

Peterson, B.M., Craine, E.R., and Strittmatter, P.A.  1978,  P.A.S.P., 90, 386.

Porcas, R.W., Urry, C.M., Browne, I.W.A., Cohen, A.M., Daintree, E.J., and
  Walsh, D.  1980,  M.N.R.A.S., 191, 607.

Richter, G.A., Richter, G.M., Richter, L., and Richter, N.B.  1974,  Astron.
  Nachr., 295, 19.

Rudnick, L. and Adams, M.T.  1979, A.J., 84, 437.

Rudnick, L. and Owen, F.N.  1977, A.J., 82, 1.

Sandage, A.  1966,  Ap.J., 145, 1.

Sandage, A.  1967, Ap.J.Lett., 150, L145.

Sandage, A.  1972, Ap.J., 178, 25.

Sandage, A., Kristian, J., and Westphal, J.A.  1976, Ap.J., 205, 688.

Sargent, W.L.W.  1973, Ap.J.Lett., 182, L13.

Schmidt, M.  1965, Ap.J., 141, 1.

Schmidt, M.  1974, Ap.J., 193, 505; 195, 253 (E).

Smith, H.E. and Spinrad, H.  1980, P.A.S.P., 94, 397.

Smith, H.E., Spinrad, H., and Smith, E.O.  1976, P.A.S.P., 88, 621.

Spinrad, H.  1982, P.A.S.P., 94, 397.

Spinrad, H., Djorgovski, S., Man, J., and Aguilar, L.  1985, P.A.S.P., 97, 932.

Spinrad, H. and Smith, H.E.  1973, Ap.J.Lett., 179, L71.

Spinrad, H., Stauffer, J., and Butcher, H.  1981, Ap.J., 244, 382.

Strittmatter, P.A., Carswell, R.F., Gilbert, G., and Burbidge, E.M.  1974,
  Ap.J., 190, 509.

Ulrich, M.H.  1976, Ap.J., 206, 364.

Vigotti, M., Grueff, G., Perley, R., Clark, B.G., and Bridle, A.H.  1989,
  A.J., 98, 419.

Walsh, D. and Carswell, R.F.  1982, M.N.R.A.S., 200, 191.

Walsh, D., Wills, B.J., and Wills, D. 1979, M.N.R.A.S., 189, 667.

Walsh, D., Beckers, J.M., Carswell, R.F., and Weymann, R.J.  1984, M.N.R.A.S.,
  211, 443.

Wilkinson, A., Hine, R.G., and Sargent, W.L.W.  1981, M.N.R.A.S., 196, 669.

Wills, B.J. and Wills, D.  1979, Ap.J.Suppl., 41, 689.

Wills, D. and Wills, B.J.  1976, Ap.J.Suppl., 31, 143.

Willson, M.A.G.  1972, M.N.R.A.S., 156, 7.