V/59 Cataclysmic Bin, Low-Mass X-ray Bin, Related obj (Ritter 1990)

Catalogue of Cataclysmic Binaries, Low-Mass X-Ray Binaries and Related Objects 5th edition

Ritter H.

<Astron. Astrophys. Suppl. Ser. 85, 1179 (1990)>

Description:

The catalogue lists coordinates, magnitudes, orbital parameters, stellar parameters of the components and other characteristic properties of 168 cataclysmic binaries, 36 low-mass X-ray binaries and 28 related objects with known or suspected orbital periods together with a comprehensive selection of the relevant literature that appeared after 1986. In addition the catalogue contains a list of references to published finding charts for 222 of the 232 objects. A cross-reference list of object designations concludes the catalogue.

Introduction:

The objects listed in this catalogue are subdivided into three main object classes, i.e. into "Cataclysmic Binaries", "Low-Mass X-Ray Binaries" and "Related Objects" The defining characteristics of the three object classes used here are the following:

c a t a c l y s m i c b i n a r i e s

Are semi-detached binaries consisting of a white-dwarf primary (or a white-dwarf precursor) and a low-mass secondary which is filling its critical roche lobe. The secondary need not necessarily be unevolved. It may even be a highly evolved star as e.g. in the cases of GP COM and AM CVN. A more detailed description of the main characteristics of these objects may be found in the following books and review articles:

Bode, M.F., Evans, A., (Eds.): 1989, Classical Novae, John Wiley & Sons ltd., Chichester

Cropper,M.: 1990, Space Sci. Rev., in press (for the Am Her stars)

la Dous, C.: 1990, in: Cataclysmic Variables and Related Objects, M. Hack, (Ed.), NASA / CNRS Monograph Series on Non-Thermal Phenomena in Stellar Atmospheres, in press

Wade, R. A.: 1985, in: Interacting Binaries, P. P. Eggleton and J. E. Pringle (Eds.), D. Reidel Publ. Co., Dordrecht

Wade, R.A., Ward, M.J.: 1985, in: Interacting Binary Stars, J.E. Pringle and R.A. Wade (Eds.), Cambridge Univ. Press, p. 129

Warner, B.: 1976, in: Structure and Evolution of Close Binary Systems, IAU Symp. no. 73, P. Eggleton, S. Mitton and J. Whelan (Eds.), D. Reidel (Dordrecht), p. 85

l o w - m a s s x - r a y b i n a r i e s

Are semi-detached binaries consisting of a neutron-star primary and a low-mass secondary which is filling its critical roche lobe. Observationally they are distinguished from the luminous massive X-ray binaries by the following main properties: in general the spectra of the low-mass x-ray binaries (at maximum light) are devoid of normal stellar absorption features. The ratio of their X-ray to optical luminosities is much larger than unity. Typically it ranges from about 100 to about 10000. A more detailed description of the main characteristics of these objects may be found in the following review articles:

Mason, K.O.: 1986, in: Physics of Accretion onto Compact Objects, Lecture Notes in Physics, Vol. 266, K.O. Mason, M.G. Watson, and N.E. White (Eds.), Springer Verlag, Heidelberg, p. 29

Mc McClintock, J.E., Rappaport, S.A.: 1985, in: Cataclysmic Variables and Low-Mass X-Ray Binaries, D.Q. Lamb and J. Patterson, (Eds.),D. Reidel Publ. Co., Dordrecht, p. 61

White, N.E., Mason, K.O.: 1985, Space Science Reviews 40, 167

R e l a t e d O b j e c t s

Are detached binaries consisting of a white dwarf primary (or a white dwarf precursor) and a low-mass secondary which is detached from its critical roche lobe. The secondary may also be a highly evolved star. for a review see e.g.

Bond, H.E.: 1985, in: Cataclysmic Variables and Low-Mass X-ray Binaries, D.Q. Lamb and J. Patterson (eds.), D. Reidel, Dordrecht, p.15

Bond, H.E.: 1989, in: Planetary Nebulae, S. Torres-Peimbert (ed.), Kluwer, Dordrecht, p. 251

Ritter, H.: 1986, Astron. Astrophys. 169, 139

According to the subdivision in these three object classes the catalogue contains three major sections. Each of the three catalogue sections is further subdivided into a catalog file, where a few characterizing parameters of the object are tabulated, and into a reference file, where a selection of references is given. Within each of the sections, the objects are listed in order of decreasing orbital period. In the corresponding reference section, however, the objects are listed in lexigraphical order.

The quantities listed in the catalog file and the corresponding abbreviations used in the table headings are described in the notes to the byte by byte descriptions below.

The catalogue is supplemented by a list giving references to published finding charts (fc) of the objects. In this file the objects of all three classes are merged and listed in lexigraphical order. In order to facilitate finding a particular object, two lists of the objects catalogued are given. The first list gives the objects in lexigraphical order, the second one in order of increasing right ascension. For each object, both lists give three page numbers for the printed file catalog.doc: the first one referring to the table section (ts), the second one to the corresponding reference section (rs) and the third one to the list giving references to the finding charts (fc). An asterisk following the name of the object indicates that the object is also known under other designations. these are cross-referenced in the "who's who ?" (whoswho.dat) file. This file includes also a list of references to various catalogue acronyms that appear in this compilation.

A more complete list of this kind may be found in "the first dictionary of the nomenclature of celestial objects" by A. Fernandez, M.-C. Lortet and F. Spite that appeared in Astron. Astrophys. Suppl. Ser. 52, Vol. 4, (1983) and in its supplements by M.-C. Lortet in Astron. Astrophys. Suppl. Ser. 64, 303-324, 325-328 (1986) and by M.-C. Lortet and F. Spite in Astron. Astrophys. Suppl. Ser. 64, 329-390 (1986).

File Summary:

Note on catalog.doc:

The first character is for Fortran carriage control ('0' is linefeed, '1' is formfeed). In order to obtain a proper printout the length of the forms should allow for up to 64 lines per page and the width sufficient to print 128 columns.

Page numbers are given in columns 128-129. The errors listed in the "note added in proof" of the original paper were corrected.

* The file can easily be transformed into a printable file on a Unix station with the shell command:

awk 'BEGIN{c[0]="\n";c[1]="\f"}{print c[substr($0,1,1)] substr($0,2)}' print

Byte-by-byte Description of file: catclysm.dat

Note on OBJECT:

Object name : wherever possible, the designation of the object given in the general catalogue of variable stars is used here.

Note on Alt:

Alternate name : Is a frequently used alternative name. Further alternative designations are given in the whoswho.dat file.

Note on RA*:

Coordinates :

Right ascension (2000.0) in hrs min sec

Declination (2000.0) in deg ' "

the coordinates are given in the following format:

right ascension: hh mm ss.s

declination : ddd mm ss a

Note on CoordAcc:

In the declination field, "a" is the accuracy of of the coordinates in seconds of arc (written as a hexadecimal number, i.e. 10" = A , 11" = B , 12" = C , 13" = D , 14" = E , 15" = F). In a case where "A" > 15" or where the accuracy of the coordinates is not known, the "CoordAcc" field is left blank.

Note on OType1, OType2, OType3, OType4:

The object type is coarsely characterized using the following abbreviations:

AC = AM CVN STAR, DOES NOT CONTAIN HYDROGEN, SUBTYPE OF NL

AM = POLAR = AM HER SYSTEM, SUBTYPE OF NL, CONTAINS A SYNCHRONOUSLY ROTATING, MAGNETISED WHITE DWARF

CP = COHERENT PULSATOR, CONTAINS A COHERENTLY PULSATING WHITE DWARF

DD = SYSTEM CONSISTS OF TWO DEGENERATE COMPONENTS

DN = DWARF NOVA

DQ = INTERMEDIATE POLAR OR DQ HER SYSTEM, CONTAINS A NON-SYNCHRONOUSLY ROTATING MAGNETISED WHITE DWARF

DS = DETACHED SYSTEM

N = CLASSICAL NOVA

NA = FAST NOVA (DECLINE FROM MAX. BY 3 MAG. IN LESS THAN ABOUT 100 DAYS)

NB = SLOW NOVA (DECLINE FROM MAX. BY 3 MAG. IN MORE THAN ABOUT 100 DAYS)

NC = EXTREMELY SLOW NOVA (TYPICAL TIME SCALE OF THE DECLINE FROM MAXIMUM: DECADES)

NL = NOVA-LIKE VARIABLE

NR = RECURRENT NOVA

PN = CENTRAL STAR OF A PLANETARY NEBULA

SU = SU UMA STAR, SUBTYPE OF DN

UG = DWARF NOVA OF EITHER U GEM OR SS CYG SUBTYPE

UX = UX UMA STAR, SUBTYPE OF NL

VY = VY SCL STAR (ANTI DWARF NOVA), SUBTYPE OF NL

XB = X-RAY BURST SOURCE

XL = LOW-MASS X-RAY BINARY, SCO X-1-LIKE

XP = X-RAY PULSAR

XS = X-RAY SOURCE

XT = TRANSIENT X-RAY SOURCE

ZC = Z CAM STAR, SUBTYPE OF DN

* = OBJECT POSSIBLY RELATED TO THE DQ HER STARS

Note on mag1, mag2, mag3, mag4:

Apparent V magnitude (B magnitude if followed by B) with the following meaning:

mag1 = maximum brightness of

NOVAE (N,NA,NB,NC,NR) IN MINIMUM

DN (UG,ZC,SU) IN MINIMUM

NL (UX,AC) IN NORMAL STATE

NL (AM,VY) IN HIGH STATE

XL (XT,XB) IN QUIESCENCE

DS OUTSIDE ECLIPSE

mag2 = minimum brightness, in case of eclipses magn. at mideclipse, of

NOVAE (N,NA,NB,NC,NR) IN MINIMUM

DN (UG,ZC,SU) IN MINIMUM

NL (UX,AC) IN NORMAL STATE

NL (AM,VY) IN HIGH STATE

XL (XB,XT) IN QUIESCENCE

DS

mag3 = maximum brightness of

NOVAE (N,NA,NB,NC,NR) IN OUTBURST

DN (UG,ZC) IN OUTBURST

DN (SU) IN NORMAL OUTBURST

NL (AM,VY) IN LOW STATE

XL (XB,XT) IN OUTBURST

mag4 = brightness of

ZC IN STANDSTILL

SU IN SUPEROUTBURST

= minimum brightness of

NL (AM,VY) IN LOW STATE

Note on T1:

for DN (UG, ZC), the typical time interval (in days) between two subsequent outbursts for DN (SU), the typical time interval (in days) between two subsequent normal outbursts for XL (XT), the typical time interval (in days) between two subsequent X-ray active states

Note on T2:

For DN (SU), the typical time interval (in days) between two subsequent superoutbursts

Note on PerOrb:

Orbital period (in days), in case of object type

DQ : the spectroscopic period is given here if it is different from the photometric one.

SU : if followed by *, the orbital period has been estimated from the known superhump period using the empirical relation given by B. Stolz and R. Schoembs (1984,Astron.Astrophys.132,187)

* : Spectroscopic Period, Photometric Period if followed by P.

Note on P2:

Second period (in days), in case of object type N, NA, NB, NC : orbital period of the prenova, unless the object is also of type DQ or *. In these cases see below.

DQ : the photometric period is given here if it is different from the spectroscopic one.

SU : superhump period. wherever possible, the superhump period at the beginning of a superoutburst is given.

* : photometric period.

Note on P3, P4:

Additional periods in the system (in seconds), in case of object type

CP :

3. PER. = period of coherent pulsation, (transient if followed by t).

4. PER. = second period of coherent pulsation, (transient if followed by t).

DQ :

3. PER. = rotation period of the white dwarf.

4. PER. = optical period, (presumably due to reprocessed x-rays).

XP :

3. PER. = pulse period of the pulsar.

4. PER. = optical period, (presumably due to reprocessed x-rays).

The occurrence of transient quasi-periodic oscillations (QPO) in objects of type N, DN, NL, XL, XT, XB and XP is indicated in the field u_P3.

Note on EB:

indicates the occurrence of eclipses if blank no eclipses observed if 1 1 eclipse per orbital revolution observed if 2 2 eclipses per orbital revolution observed if d periodic eclipse-like dips observed

Note on SB:

type of spectroscopic binary if 1 single-lined spectroscopic binary if 2 double-lined spectroscopic binary

Note on TClass, LClass:

The number indicates the luminosity class , i.e.

I = 1

II = 2

III = 3

IV = 4

V = 5

Byte-by-byte Description of file: lmxrb.dat

Please note that the notes to the fields of the table are not repeated here and can be found as notes to the description of cataclysm.dat.

Byte-by-byte Description of file: relobj.dat

Byte-by-byte Description of file: objbynam.dat, objbyra.dat

Byte-by-byte Description of file: catclref.dat, lmxrbref.dat, relatref.dat

The printed version of the catalog:

The file catalog.doc is the catalogue in print-out format. 4409 records of 132 bytes. The first character is for carriage control. In order to obtain a proper printout the length of the forms should allow for up to 64 lines per page and the width sufficient to print 128 columns. Page numbers are given in columns 128-129. The errors listed in the "note added in proof" of the original paper were corrected. The content of the complete catalog including full documentation is contained in this file. It includes a list of objects in lexigraphical order and in order by right ascension, a description of the table headings and abbreviations, the table and reference sections of the catalog, the references for the finding charts, and a list of aliases for the objects. Parts of this file have been extracted into the other data files.

For the current version of this catalogue, literature published before December 31, 1989 has, as far as possible, been taken into account.

References to previous editions:

Ritter, H.: 1982, preprint, Max-Planck-Institut fuer Physik und Astrophysik, MPA 22 (1st Edition, June 1982)

Ritter, H.: 1983, preprint, Max-Planck-Institut fuer Physik und Astrophysik, MPA 51 (2nd Edition, January 1983)

Ritter H., 1984, A&AS 57, 385 (3rd edition) (Catalogue: V/37)

Ritter H., 1987, A&AS 70, 335 (4th edition)

Acknowledgements:

The author is grateful to all the colleagues who have contributed by sending pre- and reprints of relevant papers. This work was supported in part by the Deutsche Forschungsgemeinschaft, grant KU 474/13-2.

Wanted by the author:

References to accurate coordinates and published finding charts for objects listed below. data published in easily accessible journals, catalogues and circulars, such as Acta Astron., Astron. Astrophys., Astron. J., Astrophys. J., Monthly Notices Roy. Astron. Soc., Nature, Publ. Astron. Soc. Pacific, IAU Circ., Inf. Bull. Variable Stars, etc. are strongly preferred. the requested data are needed to improve and supplement future editions of this catalogue. if you know where the data in question have been published, please send the data and the corresponding references (or only the references) to

Dr. Hans Ritter

Max-Planck-Institut fuer

Physik und Astrophysik

Karl-Schwarzschild-Strasse 1

D-8046 Garching

Germany

Accurate coordinates are needed for the following objects:

HV AND		DM DRA		CY UMA		CV IN M 67		MS1603+2600
AT CNC		CP ERI		BPM 71214		LB 1800

The accuracy of the coordinates of the following objects is either worse than 5 seconds of arc or unknown. Improved or confirmed coordinates are therefore desirable.

V1315 AQL		V664 CAS		BR LUP		DW UMA		LMC X-2		PG1026+002
V1405 AQL		V442 CEN		FY PER		EI UMA		SP 1		4U1624-49
WX ARI		V803 CEN		AY PSC		RW UMI		PG0308+096		4U1702-36
CR BOO		BW CIR		QR SGE		SS UMI		H0534-581		4U1705-44
RR CAE		TX COL		V4140 SGR		GK VIR		1E0547-7109
BY CAM		BL HYI		NN SER		QQ VUL		1H0709-36
QU CAR		DO LEO		BE UMA		GRU V1		PG0818+513

References to published finding charts, wherever possible photographic ones, are needed for the following objects:

BW CIR		CY UMA		CV IN M 67		L870-2		MS1603+2600		1H1929+509
DM DRA		BPM 71214		LB 1800		1H0709-36

References to better, i.e. photographic, finding charts would be welcome for the following objects:

HV AND

AT CNC

V425 CAS

IP PEG

FY PER

See also:

V/82 : compilation of cataclysmic binaries with known or suspected orbital periods (Ritter H., Kolb U., in "X-ray Binaries", Cambridge Astrophys. Ser. No 26)

History:

Original received from Dr. Ritter by CDS. NASA ADC converted the documentation to standard format in June 1995. The original catalogue contained 3 files: the format documentation, the catalog in print-out format and the documentation. The format documentation was reformatted and absorbed in this ReadMe file. Information from the full catalog documentation was also used to complete the ReadMe file. Tables were extracted for the low-mass X-ray binaries and related objects and reformatted. CDS added the notes about printing the print file and generated some changes to the labels and text. The contributions of ADC and CDS were combined.

(End) Francois Ochsenbein [CDS] and Paul Kuin [ADC/NASA] 25-Oct-1995