4. Notes on some individual objects

AP Cru.

This is Nova Cru 1935. It is a poorly known object discovered as a variable in 1935 and later reclassified as a nova, but without a spectroscopic confirmation (D87). The H in moderate emission in our spectrum is very sharp, its width not exceeding the instrumental PSF and very unlike those of the validated CVs (cf. Fig. 3).

V650 Ori, DE Cnc and IM Com.

Faint objects with nearly featureless (due to poor S/N) cool continua, similar to field G-K stars.

 

Name Continuum Fluxes

3450 3750 4000 4400 4800 5200 5600 6000 7050 8000 8800

V650 Ori 1.22 1.22 1.12 1.00 0.47 0.95 0.48

DE Cnc 0.69 0.78 1.02 1.20 1.00 1.24 1.28 1.21 1.08 0.93

1H 1025+220 2.53 1.92 1.75 1.38 1.14 1.00 0.85 0.74 0.53 0.40 0.32

V442 Cen 0.77 1.15 1.17 1.09 1.00 0.88 0.74 0.51

PG 1157+004 1.90 1.76 1.57 1.30 1.05 1.00 0.86 0.72 0.51 0.38 0.28

IM Com 0.43 0.89 0.99 0.94 1.18 1.00 0.93 0.92 0.74 0.58 0.45

AP Cru 0.05 0.11 0.18 0.58 0.76 1.00 1.32 1.44 1.72 2.02 1.98

V485 Cen 1.86 1.67 1.39 1.00 0.83 1.00 0.79 0.71 0.69 0.57 0.43

PG 1510+234 2.27 1.96 1.81 1.46 1.17 1.00 0.85 0.73 0.51 0.39 0.30

EK TrA 2.86 2.64 1.64 1.16 0.92 1.00 0.80 0.72 0.79 0.55 0.43

PG 1522+122 2.97 2.54 2.34 1.69 1.27 1.00 0.78 0.63 0.36 0.25 0.18

BR Lup 3.29 2.55 1.61 1.19 0.99 1.00 0.89 0.79 0.82 0.70 0.40

IM Nor 1.03 1.16 0.43 0.93 1.00 1.18 1.99 3.93

HP Nor 2.03 1.72 1.61 1.37 1.14 1.00 0.87 0.76 0.60 0.48 0.37

IK Nor 1.88 1.69 0.96 0.81 0.84 1.00 1.05 1.13 1.44 1.55 1.39

KQ Nor 0.17 0.24 0.49 0.67 0.99 1.00 1.17 1.23 1.23 1.15 0.99

LR Nor 0.27 0.45 0.67 0.81 0.96 1.00 1.11 1.18 1.13 1.10 0.84

PG 1633+115 1.72 1.50 1.65 1.41 1.17 1.00 0.86 0.73 0.53 0.41 0.32

AC Sco 1 0.14 0.25 0.48 0.72 0.95 1.00 1.09 1.12 1.03 0.92 0.76

AC Sco 2 0.15 0.28 0.45 0.61 0.87 1.00 1.19 1.32 1.48 1.56 1.49

HO Del 1.95 1.95 1.33 1.11 1.02 1.00 0.89 0.86 0.81 0.64 0.49

 

V442 Cen.

The object has been observed close to an outburst maximum, with the only emission being a faint core in the H profile.

HP Nor.

This object too has been observed during an outburst phase, half-way between maximum and quiescence as suggested by the spectral appearance and the V magnitude in Table 6 (click here). The classification among the Z Cam sub-class in DS93 could indicate that we have observed HP Nor during a stand-still phase.

PG1157+004.

The spectrum is classified as a white dwarf of the DA type. A negative detection at ( mag) was reported in Paper I. Photometry in Table 6 (click here) fits well the entries in the PG catalogue (Green et al. 1986), arguing against photometric variability.

V485 Cen.

Remarkable spectrum with He I lines rivaling in intensity with hydrogen, a chemical abundance effect. Augusteijn et al. (1996) argued for a 59 orbital period, thus our 60 exposure spectrum looks as a perfect average over the orbital period. The suggestion by Augusteijn et al. about contribution to the system emission by the secondary star in the red part of the spectrum is confirmed by the color progression in our Table 6 (click here). Tutukov & Yungelson (1996) has modeled the ultra-short orbital period binaries like V485 Cen as helium white dwarf donors and carbon-oxygen WD accretors, with important implications for supernovae and accretion induced collapses.

PG 1510+234.

The object has been photometrically confirmed as a dwarf nova with a short outburst cycle length by Iida et al. (1995), with a range in V between 14.8 and 17.9 mag. Our spectrum shows an H in moderate emission and an emission core inside a broad absorption for higher Balmer lines which is appropriate for a CV halfway between outburst maximum and quiescence, as supported by the V=16.3 mag we measured on our spectrum.

PG 1522+122.

Haefner (1995) reported the object does not show flickering activity. Our photometry in Table 6 (click here) is quite close to that reported in the PG catalogue (Green et al. 1986), suggesting limited or no variability. Our spectrum resembles that of a late sdB (HeI 4471 Å weakly present).

 

Name Classification

V650 Ori cool cont.

DE Cnc cool cont.

1H 1025+220 CV

V442 Cen CV

PG 1157+004 WD (DA)

IM Com cool cont. AP Cru

V485 Cen CV

PG 1510+234 CV

EK TrA CV

PG 1522+122 sdB

BR Lup CV

IM Nor K:

HP Nor CV

IK Nor CV

KQ Nor K3 III

LR Nor G2 II :

PG 1633+115 CV

AC Sco 1 F8 V

AC Sco 2 G5 V

HO Del CV

 

 

Name V U-B B-V

V650 Ori 20.25 0.40 0.42

DE Cnc 18.16 0.47 0.76 0.51 0.58

1H 1025+220 16.44 -0.81 0.09 0.20 0.17

V442 Cen 12.25 0.19 0.37 0.11

PG 1157+004 15.81 -0.70 0.17 0.16 0.15

IM Com 18.07 0.06 0.56 0.34 0.37

AP Cru 18.68 0.60 1.37 0.79 0.98

V485 Cen 18.06 -0.81 0.29 0.29 0.46

PG 1510+234 16.27 -0.72 0.06 0.17 0.13

EK TrA 16.50 -1.09 0.05 0.39 0.41

PG 1522+122 16.44 -0.84 -0.15 0.02 -0.13

BR Lup 18.42 -1.18 0.15 0.41 0.49

IM Nor 20.03 1.47 1.22 1.48

HP Nor 14.18 -0.75 0.15 0.24 0.30

IK Nor 17.58 -1.03 0.69 0.69 0.89

KQ Nor 13.71 0.83 1.08 0.58 0.64

LR Nor 18.28 0.29 0.92 0.55 0.62

PG 1633+115 15.95 -0.58 0.13 0.19 0.19

AC Sco 1 13.95 0.86 1.02 0.51 0.53

AC Sco 2 17.18 0.66 1.19 0.70 0.82

HO Del 17.82 -0.86 0.26 0.41 0.45

 

IM Nor.

Elliot & Liller (1972) reviewed the available very scanty photometric data on IM Nor Nova Nor 1920, which rose to mag 9 and lingered there for at least a couple of months. No spectroscopic information collected during the eruption is available. Our spectrum refers to the star marked in the finding chart by D87 and is quite featureless, possibly a K star. We measure B=21.5 on our spectrum, which is quite close to the eye-estimated mag = 22j by D87 on the SRC plates. The faintness (and therefore distance), very red colors and low galactic latitude () all suggest significant reddening. The strongest absorption line in the spectrum is in fact the (interstellar) NaI D at Å.

IK Nor.

A CV-like emission line spectrum with the TiO bands of the secondary star well visible in the red. The red-peaked energy distribution of the secondary and a low relative brightness of the disk may explain the slope of the continuum and the red colors in Table 6 (click here). Interstellar reddening does not seem to play an appreciable role due to the absence of NaI D absorption at Å.

PG 1633+115.

The spectra of Ringwald (1993) show weak H emission and even weaker H absorption. Our spectrum presents emission cores in broad H, H and H absorptions and a full emission H of moderate intensity. Misselt & Shafter (1995) reported short term mag variability of PG 1633+115 with periods and wider variability over weeks. The object looks as a genuine CV observed possibly far from flat quiescence conditions.

AC Sco.

The star marked in DS93 is an optical double. We observed both objects. The brighter star is classified as F8 V. The fainter one arcsec to the south of the bright one is a G5 V.

 
Figure 4: Spectra of BR Lup and HO Del. The offset applied for plot clarity is given in brackets next to the star name. The spectra are not corrected for reddening. The asterisk means that a boxcar smoothing (3 pixels window) has been applied. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 5: Spectra of IK Nor and V485 Cen. The offset applied for plot clarity is given in brackets next to the star name. The spectra are not corrected for reddening. The asterisk means that a boxcar smoothing (3 pixels window) has been applied. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 6: Spectrum of EK TrA (not corrected for reddening). Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 7: Spectra of HP Nor, KQ Nor and AC Sco #1. The offset applied for plot clarity is given in brackets next to the star name. The spectra are not corrected for reddening. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 8: Spectra of 1H 1025+220 and PG 1633+115. The offset applied for plot clarity is given in brackets next to the star name. The spectra are not corrected for reddening. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 9: Spectra of PG 1157+004, PG 1522+122 and PG 1510+234. The offset applied for plot clarity is given in brackets next to the star name. The spectra are not corrected for reddening. The asterisk means that a boxcar smoothing (3 pixels window) has been applied. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 10: Spectra of LR Nor, AP Cru, IM Nor and V650 Ori. The offset applied for plot clarity is given in brackets next to the star name. The spectra are not corrected for reddening. The asterisk means that a boxcar smoothing (3 pixels window) has been applied. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 11: Spectra of IM Com, DE Cnc and AC Sco #2. The offset applied for plot clarity is given in brackets next to the star name. The spectra are not corrected for reddening. The asterisk means that a boxcar smoothing (3 pixels window) has been applied. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1

 
Figure 12: Spectrum of V442 Cen. Fluxes in units of 10^-15 erg cm^-2 s^-1 Å^-1