IX/15 Einstein EMSS Survey (Gioia+ 1990, Stocke+ 1991) ============================================================================ The EINSTEIN Observatory Extended Medium-Sensitivity Survey (EMSS) Gioia I.M., Maccacaro T., Schild R.E., Wolter A.=1990ApJS...72..567G Stocke J.T., Morris S.L., Gioia I.M., Maccacaro T., Schild R.E., Wolter A., Fleming T.A., Henry J.P. =1991ApJS...76..813S ============================================================================ ADC_Keywords: X-ray sources ; Active gal. nuclei ; BL Lac objects ; Clusters, galaxy ; Galactic plane ; Mission_Name: Einstein
Limiting Sensitivity Area Covered (erg/cm**2/s) (sq. deg) 5.08E-14 0.09 6.09E-14 0.72 7.31E-14 2.54 8.78E-14 6.37 1.05E-13 15.1 1.26E-13 29.4 1.52E-13 55.2 1.82E-13 94.2 2.18E-13 139.4 2.62E-13 191.6 3.14E-13 249.5 3.77E-13 319.1 4.53E-13 402.0 5.43E-13 497.0 6.52E-13 582.9 7.83E-13 657.7 9.39E-13 711.8 1.13E-12 743.7 1.35E-12 762.7 1.62E-12 771.9 1.95E-12 775.7 2.34E-12 777.4 2.80E-12 777.9 3.36E-12 778.1 File Summary: -------------------------------------------------------------------------------- File Name Lrecl Records Explanations -------------------------------------------------------------------------------- ReadMe 80 . This file catalog.dat 194 835 EMSS Catalogue notes.dat 80 412 Notes to EMSS sources -------------------------------------------------------------------------------- See also: IX/18 : EINSTEIN extended source survey (EXSS) (Oppenheimer+ 1997) Byte-by-byte Description of file: catalog.dat -------------------------------------------------------------------------------- Bytes Format Units Label Explanations -------------------------------------------------------------------------------- 2- 14 A13 --- name *Name of EMSS source 17-18 I2 h RAh *Right Ascension (B1950.0) hours 19-20 I2 min RAm *RA minutes 21-24 F4.1 s RAs *RA seconds 25 A1 --- DE- *Declination sign (B1950.0) 26-27 I2 deg DEd *Dec degrees 28-29 I2 arcmin DEm *Dec arcmin 30-33 F4.1 arcsec DEs *Dec arcsec 35- 36 I2 arcsec e_pos *Positional Uncertainty 37- 40 I4 arcsec x *? Position offset between optical and X-ray 41- 44 I4 arcsec y *? Position offset between optical and X-ray 46- 51 F6.2 10-16W/m2 fX *X-ray flux (*1.E-13 ergs/cm**2/s or *1.E-16 W/m**2) in the 0.3-3.5 keV band 52 A1 --- ext_flag *Flagged '*' if source is extended 53- 57 F5.2 10-16W/m2 e_fX *1 sigma error on X-ray flux 59- 64 F6.2 ct/ks ctrate *Corrected IPC count rate 66- 69 F4.1 --- sn *Signal to Noise Ratio 71- 76 F6.1 --- cts *Uncorrected net counts in 0.2-3.5 keV 78- 81 F4.1 --- e_cts *Error on net counts 83- 87 I5 s live *Corrected exposure time 89- 93 F5.1 --- bkgcts *Total background counts 95- 99 I5 --- seqno *IPC sequence number of the image used 101-104 I4 --- cts_ext *? Net extended counts 106-111 F6.4 10+25m-2 nH *Hydrogen column density (*E+25 m^-2 or *E+21 cm^-2) 113-117 F5.2 mag Vmag *? Visual magnitude 119 A1 --- n_fR '<' for upper limit in fR 120-125 F6.1 mJy fR *? Radio flux at 5 GHZ 127-131 F5.2 --- fX/fv *? Logarithm of X-ray to visual flux ratio 133-136 A4 --- class *Proposed identification class of the X-ray source (see below) 138-141 A4 --- r_class *Reference for class 143-147 F5.3 --- z *? Redshift 149 A1 --- n 'n' if a note on the source is in file notes 151-194 A44 --- comment *Miscellaneous information on the source--------------------------------------------------------------------------------
(a) For the AGN, BL Lac objects and unidentified sources; we have multiplied the corrected count rate given in the ctrate column by a conversion factor appropriate for a power law spectrum with an energy index alpha = 1.0 and with the measured Galactic hydrogen column density in the direction of each IPC pointing.
(b) For unresolved galaxies and clusters of galaxies; the flux has been computed using an identical procedure but with a different conversion factor appropriate for a Raymond-Smith thermal spectrum (Raymond and Smith, 1977) with temperature of about 6 keV.
The above assumptions are justified by the results of the analysis of the X-ray energy distribution of the EMSS sources performed by Maccacaro et al. (1988). A number of sources are resolved even with the moderate angular resolution of the IPC. They are mainly clusters of galaxies but also 3 galaxies, 8 AGN, and 3 BL Lacs.
For the extragalactic population, the X-ray flux listed has been corrected ("de-reddened") for Galactic absorption. For stars we have adopted a constant conversion factor of 1 IPC count/s = 2E-11 erg/cm**2/s corresponding to a Raymond-Smith thermal spectrum with temperatures in the range 8E05 - 3E06 K and no correction for the hydrogen column density. Note that RS CVn and K and M flare stars usually have a second temperature component in the range 1 - 2E07 K which results in nearly identical conversion factors to those derived from the Raymond-Smith models over these temperature ranges (see also Fleming, 1988, for a discussion of flux estimate of X-ray selected stars).
In the case of clusters of galaxies the flux estimate should be evaluated in a region of constant physical size (e.g. 1 Mpc). Such a procedure cannot be applied to the serendipitous EMSS clusters, especially to the nearby ones, given their proximity to the ribs (or edges) of the detector or, in some cases, to the target of the observation. For all the resolved sources identified with clusters of galaxies or galaxies, and flagged as extended in the ext_flag column, we have used the extended counts measured according to the procedure described below the cts_ext column to compute the flux.
If the ext_flag column is flagged with an asterisk ('*') then extended counts from the column cts_ext were used to calculate the X-ray flux. The cts_ext column gives the net extended counts. For IPC sources, this means that counts were computed manually to include all counts belonging to the source. For sources resolved by the IPC, the observed counts have been computed manually within a region centered on the source and with a size evaluated case by case so as to contain all the counts belonging to the source itself. Background counts for these sources have been computed within this same area from the background map produced by the REV.1 processing. In these cases only the vignetting and mirror scattering corrections have been applied.
At the edge of the IPC detector the point spread function becomes significantly degraded so that some sources appear to be extended even though they might not be. Observations with a higher resolution instrument (e.g. the HRI or ROSAT) are needed to decide whether the extension is true or an artifact of the degradation of the IPC point spread function. This distortion of the point spread function cannot be modeled easily, so indications that sources are extended when they are near the IPC edge cannot be always trusted. Since these sources include ones which are identified as AGN and BL Lac objects as well as clusters, the indication of extension should be regarded as tentative.
AGN = Active Galactic Nucleus (quasar or Seyfert galaxy) CL = Cluster of galaxies *CL* = Cooling flow galaxy BL = BL Lac object GAL = "normal" galaxy STAR = star UNID = source still unidentified
References in column r_class of emss table: (MSS1) Stocke, J.T., Liebert, J., Gioia, I.M., Griffiths, R.E., Maccacaro, T., Danziger, I.J., Kunth, D., & Lub, J., 1983, ApJ, 273, 458 (1983ApJ...273..458S)
(MSS2) Gioia, I.M., Maccacaro, T., Schild, R.E., Stocke, J.T., Liebert, J.W., Danziger, I.J., Kunth, D., & Lub, J., 1984, ApJ, 283, 495 (1984ApJ...283..495G)
(1) White, S., Silk, J., & Henry, J.P., 1981ApJ...251L..65W
(2) Margon, B., Downes, R., & Chanan, G., 1985ApJS...59...23M
(3) Pravdo, S., & Marshall, F., 1984ApJ...281..570P
(4) Huchra, J., Davis, M., Latham, D., & Tonry, J., 1983ApJS...52...89H
(5) Hewitt, A., & Burbridge, G., 1987ApJS...63....1H
(6) Kriss, G., & Canizares, C., 1982ApJ...261...51K
(7) Wolstencraft, R., Hu, W., Arp, H., & Scarrott, S., 1983,, MNRAS, 1983MNRAS.205...67W
(8) Chanan, G., Margon, B., & Downes, R., 1981ApJ...243L...5C
(9) Mundt, R., Walter, F., Feigelson, E., Finkenzeller, V., Herbig, G., & Odell, A., 1983ApJ...269..229M
(10) Henry, J.P., Soltan, A., Briel, U., & Gunn, J., 1982ApJ...262....1H
(11) Margon, B., Boronson, T., Chanan, G., Thompson, I., & Schneider, D., 1986PASP...98.1129M
(12) Caillault, J., Helfand, D., Nousek, J., & Takalo, L., 1986, 1986ApJ...304..318C
(13) Morris, S., Schmidt, G., Liebert, J., Stocke, J., Gioia, I., & Maccacaro, T., 1987ApJ...314..641M
(14) Biermann, P., Schmidt, G., Liebert, J., Stockman, H., Tapia, S., Strittmatter, P., West, S., & Lamb, D., 1985ApJ...293..303B
(15) Reichert, G., Mason, K., Thorstensen, J., & Bowyer, S., 1982, 1982ApJ...260..437R
(16) J. Huchra & M. Postman (private communication)
(17) de Vaucouleurs, G., de Vaucouleurs, A., & Corwin, H., 1976,
Second Reference Catalogue of Bright Galaxies (Austin:
University of Texas Press) (Cat.
(18) I.J. Danziger (private communication)
(19) Maccagni, D., Garilli, B., Gioia, I.M., Maccacaro, T.
Vettolani, G., & Wolter, A., 1988ApJ...334L...1M
(20) Katgert, P., Thuan, T., & Windhorst, R., 1983ApJ...271....1K
(21) Mason, K., Spinrad, H., Bowyer, S., Reichert, G., & Stauffer,
J., 1981AJ.....86..803M
(22) Hoessel, J., Gunn, J., & Thuan, T., 1980ApJ...241..486H
(23) F. Walter (private communication)
(24) Morris, S.L., Liebert, J., Stocke, J.T, Gioia, I.M., Maccacaro,
T., Schild, R.E., & Wolter, A., 1990, ApJ, 383, 686
(1990ApJ...365..686M)
(25) Chanan, G., Margon, B., Helfand, D., Downes, R., & Chance, D.,
1982ApJ...261L..31C
(26) Kowalski, M., Ulmer, M., & Cruddace, R., 1983ApJ...268..540K
(27) Nesci, R., Gioia, I., Maccacaro, T., Morris, S., Perola, G.,
Schild, R., & Wolter, A., 1989ApJ...344..104N
(28) Maia, M., DeCosta, L., Willmer, C., Pellegrini, P., & Rite, C.,
1987AJ.....93..546M
(29) Marschall, L., Stefanik, R., Nations, R., & Karshner, G., 1989,
BAAS, 21, 1083 (1989BAAS...21.1083M)
(30) Fleming, T.A., Gioia, I.M., & Maccacaro, T., 1989AJ.....98..692F
(31) Robb, R., 1989, IBUS, Nos. 3346 and 3370
(32) R. Robb, private communication;
(33) Carter, B., Inglis, I., Ellis, R., Efstathiou, G., & Godwin, J.,
1985MNRAS.212..471C
(34) Kurtz, M., Huchra, J., Beers, T., Geller, M., Gioia, I.M.,
Maccacaro, T., Schild, R., & Stauffer, J., 1985AJ.....90.1665K
(35) Silva, D., Liebert, J., Stocke, J.T. & Aaronson M., 1985,
1985PASP...97.1096S
Fleming, T.A. 1988, Ph. D. Thesis, University of Arizona
Gioia, I.M., Maccacaro, T., Schild, R.E., Stocke, J.T., Liebert, J.W.,
Danziger, I.J., Kunth, D., & Lub, J., 1984ApJ...283..495G
Gioia, I.M., Maccacaro, T., Morris, S.L., Schild, R.E., Stocke, J.T., Wolter,
A., & Henry, P.H., 1990ApJS...72..567G
Heiles, C. and Cleary, M.N., 1979, Australian J.Pys. Ap. Suppl, 47, 1.
Maccacaro, T., & al. 1982ApJ...253..504M
Maccacaro, T., Gioia, I.M., Wolter, A., Morris, S.L., & Stocke, J.T., 1988,
1988ApJ...326..680M
Raymond, J.C. & Smith, B.W., 1977ApJS...35..419R
Stark, A.A., Heiles, C., Bally, J., and Linker, R., 1989, Bells Lab,
privately distributed magnetic tape
Stocke, J.T., Liebert, J., Gioia, I.M., Griffiths, R.E., Maccacaro, T.,
Danziger, I.J., Kunth, D., & Lub, J., 1983ApJ...273..458S
Stocke, J.T., Morris, S.L., Gioia, I.M., Maccacaro, T., Schild, R.E.,
Wolter, A., Fleming, T.A., & Henry, J.P., 1991ApJS...76..813S
Contact: Isabella Gioia, Institute for Astronomy;
gioia@galileo.ifa.hawaii.edu
Note on z:
If the counterpart is extragalactic the redshift is listed (+/- 0.003).
Note on comment:
This column gives miscellaneous information on the source (i.e.
radio catalogued source, SAO name, X-ray variable source, IRAS source,
EXOSAT source, etc.). The EXOSAT CMA position is reported with the
positional accuracy in parentheses. EMSS sources already published as
part of the MSS samples are labelled as MSS1 (Maccacaro et al. 1982
and Stocke et al. 1983) and MSS2 (Gioia et al. 1984).
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History and Modifications:
* 19-Jan-1993: Original version received from Isabella Gioia, table
adapted by F.Ochsenbein[CDS]
* 19-Jan-1993. Documentation reformatted to v1.4 of standard by
Paul Kuin [ADC] 31-Jul-1995.
* 29-Aug-1997: catalogue number changed from VII/152 to IX/15
(high energy data)
References:
Cleary, M.N., Heiles, C., and Haslam, C.G.T., 1979A&AS...36...95C
I.Gioia, F.Ochsenbein, P. Kuin 31-Jul-1995