WGA J0043.3-2638 Since being selected for the DXRBS sample, this source was
WGA J0043.3-2638 observed by Cristiani et al. (1995A&AS..112..347C) and Wolter,
WGA J0043.3-2638 Ruscica, & Caccianiga (1998MNRAS.299.1047W), both of whom
WGA J0043.3-2638 identify it as a quasar at z=1.002. Both this redshift and the
WGA J0043.3-2638 redshift we list in Table 3 (z=0.451) have problems reproducing
WGA J0043.3-2638 some of the features found in both spectra. For example, ifthe
WGA J0043.3-2638 object is at z=1.002, it is difficult to explain the likely
WGA J0043.3-2638 emission line at4050{AA}, which we have classified as Mg II at
WGA J0043.3-2638 z=0.451. Further observations areneeded to determine the
WGA J0043.3-2638 correct redshift of this object. The rest-frame equivalent
WGA J0043.3-2638 width of the 4050{AA} emission line is 9.6{AA} (if z=0.451) or
WGA J0043.3-2638 7.0{AA} (if z=1.002), only slightly above the dividing line
WGA J0043.3-2638 between BL Lac object and FSRQ. Therefore, even though the line
WGA J0043.3-2638 is clearly broad (FWHM=3800km/s), this object is similar to
WGA J0043.3-2638 objects such as Mrk 501 and BL Lac that share this property and
WGA J0043.3-2638 must be classified as a BL Lac object.
WGA J0100.1-3337 The single emission line, which we classify as Mg II at
WGA J0100.1-3337 z=0.875, is clearly broad (FWHM=2900km/s), but its equivalent
WGA J0100.1-3337 width is close to the BL Lac/FSRQ dividing line
WGA J0100.1-3337 W_{lambda}_=9.8{AA} rest frame). We classify this object as a
WGA J0100.1-3337 BL Lac object, similarly to WGA J0043.3-2638 (see above
WGA J0100.1-3337 discussion).
WGA J0204.8+1514 This source, also known as 4C 15.05, has a radio flux above 3Jy
WGA J0204.8+1514 and was also previously observed by Stickel et al.
WGA J0204.8+1514 (1996A&AS..115....1S), who classified the source as an AGN at
WGA J0204.8+1514 z=0.833 based upon the identification of two lines as O II
WGA J0204.8+1514 {lambda}3727 and Ne I {lambda}3833. These lines are also
WGA J0204.8+1514 present in our spectrum, as are four others (Fig. 2). However,
WGA J0204.8+1514 the redshift claimed by Stickel et al. (1996A&AS..115....1S) is
WGA J0204.8+1514 likely incorrect, as all six lines cannot be accounted for if
WGA J0204.8+1514 the redshift is z=0.833. We believe that a better fit is
WGA J0204.8+1514 obtained with a redshift z=0.405. This object is also the
WGA J0204.8+1514 likely counterpart of the EGRET source 2E G0204+1514 (Thompson
WGA J0204.8+1514 et al., 1995ApJS..101..259; Mattox et al., 1997ApJ...481...95).
WGA J0210.0-1004 This object, at z=1.976, is ~2' from MS 0207.4-1016, identified
WGA J0210.0-1004 by Stocke et al. (1991ApJS...76..813S) as a radio-quiet QSO
WGA J0210.0-1004 [F(6cm)>=0.3mJy at 3{sigma}] at z=1.970. A 6cm VLA survey
WGA J0210.0-1004 performed during the EMSS project showed that there are two
WGA J0210.0-1004 fairly strong radio sources that likely would be in the PMN
WGA J0210.0-1004 beam (J. T. Stocke 1997, private communication). The stronger
WGA J0210.0-1004 source, with a flux of 133mJy, is at the position of WGA
WGA J0210.0-1004 J0210.0-1004; however, there is another 70mJy source at a
WGA J0210.0-1004 position that is not consistent with either WGA J0210.0-1004 or
WGA J0210.0-1004 MS 0207.4-1016. Even with this reduced 6cm flux, WGA
WGA J0210.0-1004 J0210.0-1004 is still a flat-spectrum source ({alpha}_r_=0.58).
WGA J0210.0-1004 There is no question about the correctness of either X-ray
WGA J0210.0-1004 source identification, since WGACAT lists a 0. 01count/s X-ray
WGA J0210.0-1004 source at a position consistent with MS 0207.4-1016 (in
WGA J0210.0-1004 addition to WGA J0210.0-1004). It is possible, however, that
WGA J0210.0-1004 X-ray emission from both sources may have contributed to the
WGA J0210.0-1004 EMSS X-ray flux. What is particularly interesting is that these
WGA J0210.0-1004 two objects are at essentiallythe same redshift and are
WGA J0210.0-1004 therefore likely associated with one another in a group or
WGA J0210.0-1004 cluster of galaxies, since the projected separation between
WGA J0210.0-1004 them is 1.6Mpc.
WGA J0245.2+1047 This object is difficult to classify because of the
WGA J0245.2+1047 largeequivalent width of its H{alpha} emission line (19.1{AA};
WGA J0245.2+1047 rest frame). However, when combined with its low Ca H and K
WGA J0245.2+1047 break strength (C=0.26) it rests securely in the BL Lac area of
WGA J0245.2+1047 the W_{lambda}_, C)-plane as defined by Marcha et al.
WGA J0245.2+1047 (1996MNRAS.281..425M). We therefore classify this object as a
WGA J0245.2+1047 BL Lac object.
WGA J0313.9+4115 The H_{alpha}_ emission line in this object's spectrum is not
WGA J0313.9+4115 very broad, exhibiting FWHM=1780km/s. The rest-frame equivalent
WGA J0313.9+4115 width of this line is close to the BL Lac/FSRQ dividing line
WGA J0313.9+4115 (13.0{AA} rest frame). The Ca IIbreak strength is 0.38, close
WGA J0313.9+4115 to the BL Lac/radio galaxy border we are using. Wehave
WGA J0313.9+4115 classified this source as a BL Lac object, but we note that the
WGA J0313.9+4115 1{sigma} errors on our measurement of C are not small enough to
WGA J0313.9+4115 exclude the alternate classification as a radio galaxy (Fig.
WGA J0313.9+4115 1). A higher S/N spectrum of this object is clearly necessary
WGA J0313.9+4115 to confirm its nature.
WGA J0340.8-1814 The H_{alpha}_ emission line in the spectrum of this object has
WGA J0340.8-1814 a rest-frame equivalent width of 16.0{AA}, and its Ca II break
WGA J0340.8-1814 strength is C=0.40. Thus it is right on the borderline of the
WGA J0340.8-1814 BL Lac region of the(W_{lambda}_, C)-plane. We have classified
WGA J0340.8-1814 this object as a radio galaxy; however, a higher S/N spectrum
WGA J0340.8-1814 is clearly necessary to confirm its nature.
WGA J0421.5+1433 Our spectra show no clear lines; however, because of its low
WGA J0421.5+1433 S/N (~7), the 2{sigma} upper limits that can be placed on its
WGA J0421.5+1433 break strength (C<0.30) and equivalent width of emission lines
WGA J0421.5+1433 (W_{lambda}_<8.2{AA}) are not very stringent. They are
WGA J0421.5+1433 adequate, however, to allow us to classify this source as a BL
WGA J0421.5+1433 Lac object. Better observations are clearly necessary.
WGA J0428.8-3805 This object has no detectable emission lines in its spectrum
WGA J0428.8-3805 (2{sigma} upper limit=0.7{AA}), and a weak Ca break (C=0.32).
WGA J0428.8-3805 We classify it as a BL Lac object using the Marcha et al.
WGA J0428.8-3805 (1996MNRAS.281..425M) criteria.
WGA J0449.4-4349 This bright BL Lac object was observed as a target by ROSAT;
WGA J0449.4-4349 however, until now it was unidentified. Because of its
WGA J0449.4-4349 nonserendipitous observation by ROSAT, we will not include it
WGA J0449.4-4349 in computations of the luminosity function. We include it here
WGA J0449.4-4349 as it was identified during our observingcampaign, and there
WGA J0449.4-4349 will probably be no other opportunity to discuss it.
WGA J0500.0-3040 We have termed this object a radio galaxy, despite the fact
WGA J0500.0-3040 that all of its emission lines have equivalent widths greater
WGA J0500.0-3040 than 5{AA} (some are as large as 70{AA}), since all are
WGA J0500.0-3040 relatively narrow (FWHM~1000-2000km/s).However, there is no
WGA J0500.0-3040 detectable 4000{AA} break in its spectrum, which points to an
WGA J0500.0-3040 unusually strong nonthermal contribution.
WGA J0513.8+0156 The Ca II break strength (C=0.34) and lack of emission lines
WGA J0513.8+0156 (2{sigma} upper limit on W_{lambda}_=1.3{AA}) allow us to
WGA J0513.8+0156 classify this source as a BL Lac object. However, the low S/N
WGA J0513.8+0156 of its spectrum blueward of the Ca II break results in a
WGA J0513.8+0156 relatively large 1{sigma} error on its break strength, large
WGA J0513.8+0156 enough so that we cannot exclude the alternate classification
WGA J0513.8+0156 as a radio galaxy (Fig. 1). A higher S/N spectrum of this
WGA J0513.8+0156 source is required to confirm its nature.
WGA J0558.1+5328 The H_{alpha}_ emission line in this object's spectrum is not
WGA J0558.1+5328 very broad, exhibiting FWHM=2100km/s. The equivalent width of
WGA J0558.1+5328 this line is closeto the BL Lac/FSRQ dividing line (9.8{AA}).
WGA J0558.1+5328 The Ca II break strength is 0.29. Weclassify this source as a
WGA J0558.1+5328 BL Lac object. However, the low S/N of its
WGA J0558.1+5328 spectrum,particularly blueward of the Ca II break (~5, compared
WGA J0558.1+5328 with ~12-15 redward of the break) does not quite allow us to
WGA J0558.1+5328 exclude the alternate (radio galaxy) classification. A higher
WGA J0558.1+5328 S/N spectrum would clarify this question.
WGA J0624.7-3230 The emission-line and absorption-line redshifts of this
WGA J0624.7-3230 objectare somewhat different (z_abs_=0.252 and z_em_=0.275).
WGA J0624.7-3230 Therefore, it is likely that the galactic emission in the
WGA J0624.7-3230 spectrum is caused by a foreground galaxy superposed upon the
WGA J0624.7-3230 radio source. The sole emission line has a rest-frame
WGA J0624.7-3230 equivalent width of 8.5{AA}, slightly over the BL Lac/FSRQ
WGA J0624.7-3230 dividing line, but the line is narrow (FWHM=900km/s). We are
WGA J0624.7-3230 classifying it as a BL Lac object, because of its small
WGA J0624.7-3230 equivalent width emission line and low Ca H and K break
WGA J0624.7-3230 contrast (C=0.22).
WGA J0656.3-2403 There is a possible emission feature in the spectrum of this
WGA J0656.3-2403 object at 3845{AA}. It is unclear whether this is a real
WGA J0656.3-2403 emission line, noise, or a cosmic ray, because of the noisiness
WGA J0656.3-2403 of the spectrum in this range. The lack of other emission lines
WGA J0656.3-2403 in the spectrum and high noise level in the blue make it
WGA J0656.3-2403 somewhat doubtful that this feature is truly an emission line.
WGA J0656.3-2403 However, if it was caused by Mg II emission, the redshift of
WGA J0656.3-2403 this object would be z=0.371, and it would be narrow
WGA J0656.3-2403 (FWHM=500km/s). We classify this source as a BL Lac object
WGA J0656.3-2403 because of the likely lineless nature of its spectrum, though
WGA J0656.3-2403 we note that if the 3845{AA} feature is indeed an emission line
WGA J0656.3-2403 it exceeds by more than a factor of 4 the traditional BL
WGA J0656.3-2403 Lac/FSRQ dividing line (rest-frame W_{lambda}_=24.5{AA}).
WGA J0724.3-0715 Despite its faintness, the H_{alpha}_ emission line in the
WGA J0724.3-0715 spectrum of this object is quite broad (rest-frame
WGA J0724.3-0715 W_{lambda}_=30.3{AA}, FWHM=4000km/s). We therefore classify it
WGA J0724.3-0715 as an FSRQ.
WGA J0744.8+2920 This object was identified independently by Gregg et al.
WGA J0744.8+2920 (1996AJ....112..407G) as part of the FIRST Bright Quasar Survey
WGA J0744.8+2920 (FBQS, and by Wolter et al. (1998MNRAS.299.1047W). We confirm
WGA J0744.8+2920 both identifications and redshifts; however, a comparison of
WGA J0744.8+2920 our spectrum with that given by Wolter et al. reveals a large
WGA J0744.8+2920 deficit in the blue in our spectrum. This is most likely aused
WGA J0744.8+2920 by a combination of instrumental and weather-related factors.
WGA J0816.0-0736 We tentatively classify this source as a BL Lac object, because
WGA J0816.0-0736 of its lack of emission lines and low break strength (C=0.37).
WGA J0816.0-0736 However, on account of the low S/N of its spectrum blueward of
WGA J0816.0-0736 the Ca II break (~4 compared with ~20 above 5000{AA}), we
WGA J0816.0-0736 cannot exclude the alternative (radio galaxy) classification,
WGA J0816.0-0736 because of the large 1{sigma} error on C(0.18). A higherS/N
WGA J0816.0-0736 spectrum is required to clarify its nature.
WGA J0900.2-2817 A second spectrum of this object, with much wider wavelength
WGA J0900.2-2817 coverage, was obtained in 1997 May at the ESO 2.2 m telescope.
WGA J0900.2-2817 That spectrum (which will be published in a later paper)
WGA J0900.2-2817 confirms the identification of the single line as Mg II
WGA J0900.2-2817 {lambda}2798.
WGA J1057.6-7724 The fairly low S/N spectrum we have (S/N~7) places
WGA J1057.6-7724 2{sigma}limits on C and W_{lambda}_ that are sufficient to
WGA J1057.6-7724 classify this source as a BL Lac object. A higher S/N spectrum
WGA J1057.6-7724 is required to obtain a redshift.
WGA J1222.6+2934 The fairly low S/N spectrum we have (S/N~6) places
WGA J1222.6+2934 2{sigma}limits on C and W_{lambda}_ that are sufficient to
WGA J1222.6+2934 classify this source as a BL Lac object. A higher S/N spectrum
WGA J1222.6+2934 is required to obtain a redshift.
WGA J1525.3+4201 This source was listed as a BL Lac candidate by Ruscica et al.
WGA J1525.3+4201 (1996IAUS..175..271 R). However, our spectrum shows strong,
WGA J1525.3+4201 broad lines, and we identify his object as a quasar at z=1.189.
WGA J2317.9-4213 This object is most likely a radio galaxy, based upon its
WGA J2317.9-4213 strong Ca II break (C=0.52). It is probably associated with a
WGA J2317.9-4213 group of galaxies at the same redshift found by the Las
WGA J2317.9-4213 Campanas Redshift Survey (Schechtman et al.,
WGA J2317.9-4213 1996ApJ...470..172S).
WGA J2322.0+2114 This object was also observed by Wolter et al.
WGA J2322.0+2114 (1998MNRAS.299.1047W).We confirm both their identification and
WGA J2322.0+2114 redshift.