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 as0218+399A 1
0218+399B 2since 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.