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1971ApL.....9...53Swarup+ list 1 ADS
1973ApL....14...31Kapahi+ list 2 ADS
1973AJ.....78..673Kapahi+ list 3 ADS
1973AJ.....78.1023Joshi+ list 4 ADS
1974AJ.....79..515Kapahi+ list 5 ADS
1979MmASI...1....2Subrahmanya & Gopal-Krishna list 6 ADS
1979MmASI...1...14Singal+ list 7 ADS
1979MmASI...1...25Venkatakrishna & Swarup: list 8 ADS
1980MmASI...1...49Joshi & Singal: list 9 ADS
1987A&AS...69...91Singal list 10 ADS
(digitized by H. Andernach, 5/96, typed S.Trushkin)
Ooty Lunar Occultation Surveys
1979MmASI...1....2 Subrahmanya & Gopal-Krishna: Ooty list 6
Abstract
Lunar occultations of 100 radio sources observed at 327 MHz have been
used to derive their position and structure. The flux densitries of the
source range from 0.2 to 3.7 Jy with a median value of 0.7 Jy at 327 MHz,
and a resolution of 6 arc sec has been achieved for 60 sources.
Optical identifications have been attempted for sources lying outside the
galatic plane (b >10^o) using the Polamar Sky survey prints. The derived
structure of the double source OTL 1107+036 has enabled us to suggest
its identification with a 17 mag blue galaxy instead of the previos
identification with a nearby NSO based on the positional coincidence.
All but 27 sources have been resolved in at least one scan.
The paper also included a breif summary of the 293 sources whose
occultations were observed with the Ooty radio telescope during 1970-71.
1979MmASI..14....2Singal+
Ooty Lunar Occultation observations of 65 radio sources at 327 MHz:
List 7
Abstract
Lunar occultations 327 MHz are presented for 65 radio sources observed
having median flux density of about 1.2 Jy.
A resolution of <4 arc sec has been achieved for about half of these sources
and 23 of the sources are optically identified.
The sample cantains 5 flat spectrum sources, 3 of which are quasars showing
flux variations at centimetre wavelengths. One of the quasars, viz. 1055+018
is also a metre-wavelength variable and it is found to be a compact double
source at 327 MHz.
Ooty Lunar Occultation observations of 122 radio sources at 327 MHz:
List 8
1979MmASI..25....2Venkatakrishna&Swarup
Abstract
Accurate positions, structure and identifications are presented for 122
radio sources based on their lunar occultations 327 MHz.
Most of these source have flux densities less than 1 Jy at 327 MHz.
About 60 % of the sources have been resolved. Optical identifications have
been suggested for 23 sources. Two of the identified galaxies lie in
the directions of Abell clusters. There a re two BSO's of about 18 mag
in the close proximity to the radio source 0738+178. Nine sources
have flat spectra and one source has a synchrotron self-absorbed spectrum.
A preliminary comparison indicates that the structure of the weaker sources
of flux density S_327 ~ 2 Jy is similar to that of the high-luminosityColumn
3CR sources.
1980MmASI...1...49Joshi & Singal
OOTY LUNAR OCCULTATION SURVEY: LIST 9
Mohan N. Joshi and Ashok K. Singal
In this paper we present position and structure information at 327 MHz for
240 radio sources derived from their lunar occultation observations made
with the Ooty radio telescope. The flux densities of the sources lie in the
range 0.2 to 4.5 Jy with a median value of 0.7 Jy. Resolutions of 6 arcsec
or better have been achieved for more than 5000 of the sources. A search for
optical identifications using the Palomar Sky Survey Prints was Made for
all the sources and the results are presented. A brief description of the
flat spectrum sources found in the Ooty Occultation Survey is given. The
steps that are currently being taken to improve the sensitivity of the
Ooty radio telescope are briefly described.
1987A&AS...69..91Singal: Ooty list 10
Ooty lunar occultation survey of radio sources
Abstract
We present here accurate radio positions and the arcsec angular
structural infirmation for 239 radio sources. The information is derived
from the lunar occultation observation made at 327 MHz using the Ooty radio
telescope.
...
Column description taken from list 6
- 1. Source name in the standard convention, with the prefix OTL.
An asterisk (*) indicates that additional notes or comments are
given in the text for the same source.
- 2. Total number of occultations used; a single immersion or emersion
is called an occultation.
- 3. Name of the individual component of a source, if it is not single.
The components are named A,B,C in the order of increasing right
ascension. The code 'S' indicates that the entries correspond to the
source being single in that particular scan, but that the overall
structure was different in another scan.
- 4. Flux density S_327MHz for the source and its components. The total flux
density is given in the first row, followed by the flux density of the
components mentioned in column 3 for double or triple sources.
- 5. Position angle of scan (PA) in degrees
- 6. The effective resolution
- 7. The derived angular size of the source or one of its components along
the PA mentioned in col. 5.
- 8-10. Similar to columns 5,6 and 7, respectively, but corresponding to
another available scan.
- 11-12. Overall structure of the source. The derived largest angular size (LAS)
is entered in column 11, with the position angle of separation of
double sources in column 12.
- 13. Abbreviated notes to the source structure. The following abbreviations
are used:
U = unresolved S = single; D = double; PD = possibly double;
HT = head-tail; CH = core - halo; T = triple, showing a central component;
BrN% = bridge with the percentage flux as indicated;
Cx = a more complex structure that the above mentioned classes.
An abbreviation followed by an asterisk (*) indicates that the
interpretation was based on the 'optimum deconvolution method' (ODM).
- 14,15,16. RA, DEC and their standard errors are given in cols. 15 and 16,
respectively. The centroid of a double source is indicated by the
symbol 'CN' in column 14. The symbol 'a' under position errors implies
that the errors are better specified along two mutually perpendicular
position angles given in the footnotes to the table.
- 17,18. The difference in the optical position from the radio centroid or
from that of the corresponding component listed in column 14. The
optical positions are generally given only if the radio-optical
difference is less than 15", but sometimes more distant objects are also
included if the source has large angular extent or the object is
situated in the boundary of the source within the position errors.
Optical positions are generally accurate to 0.5 arcsec, but those
enclosed in brackets [or followed by a colon in the electronic version]
have larger errors of about 2 arcsec in each coordinate.
- 19. Photographic magnitude of the optical object, estimated visually from the
Sky Survey prints and may be in error by +-1 mag.
- 20. Notes on the optical objects. Positive or likely identifications are
indicated by a hash (#). The following abbreviations are used.
EF = empty field; BSO = blue stellar object; RSO = red stellar object;
NSO = neutral stellar object; G = galaxy; RG = red galaxy;
BG = blue galaxy; DG = double galaxy; EG = elliptical galaxy;
NG = N galaxy; db = dumb-bell type galaxy;
RO = red object; BO = blue object; QSO = quasi stellar object;
Cwd = crowded field; Cl = cluster;
INP = identification not possible because of large errors in radio
position or due to presence of more than one optical object within
the radio boundary;
Def? = could be a defect on the photographic plate.
- 21. absolute value of galactic latitude |b2| of the source, in degrees
- 22. Other catalogue names. If the source is listed in several catalogues,
only one catalogue name is generally given.