NGC 1136 – Higher redshift companion

NGC 1136 was included to the sample of Arp (1981). Arp described the system as disturbed spiral with disturbed companion. He wrote:

The central spiral has strong, disturbed arms. The companion is relatively bright and strongly distorted. The spectral characteristics of the companion are younger. This is a prototype example of a spiral with an apparently physically associated companion.

However, the companion (NGC 1135) has radial velocity of 13339 km/s while the main galaxy has radial velocity of 5610 km/s – too large difference for this system to be traditionally considered as physically interacting pair. This system was also included to the analysis of Arp (1982) and Soares et al. (1995).

Notes

– There are not many objects with available redshift near NGC 1136 in NED (NASA Extragalactic Database). In addition to NGC 1136 and NGC 1135 there’s only one QSO (object 3, not shown in Figure 1), which is 9.2 arcminutes from NGC 1136. The QSO is rather bright one with B band apparent magnitude of 15.4.


Figure 1. The objects with measured redshifts near NGC 1136. Size of the image is 10 x 10 arcmin. Image is from Digitized Sky Survey (POSS2/UKSTU Blue).

Objects and their data

NBR NAME TYPE REDSHIFT MAG SEPARATION
1 NGC 1136 SAB(rl)ab 0.018713 (5610 km/s) 13.75 0
2 NGC 1135 Sd? pec 0.044494 (13339 km/s) 16.16 2.932
3 SUMSS J024958-550315 QSO 0.230000 15.4 (B) 9.219

NED objects within 10′ from NHC 1136

References

Arp, 1981, ApJS, 46, 75, “Spectroscopic measures of galaxies, their companions, and peculiar galaxies in the southern hemisphere”

Arp, 1982, ApJ, 256, 54, “Characteristics of companion galaxies”

Soares et al., 1995, A&AS, 110, 371, “Southern binary galaxies. I. A sample of isolated pairs”

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NGC 5107 – QSO at minor axis

NGC 5107 is a companion galaxy to NGC 5112. Arp (1981) included this system to his set of new quasars near companion galaxies. He wrote:

Figure 15 (Plate 11) shows that very close to this companion a new quasar has been discovered.

(The quasar in question is object 2 in Figure 1 below.) Burbidge et al. (1990), Burbidge (1996), and Bukhmastova (2001) included this system within their sample of associations between QSOs and galaxies.

In addition to these papers, this system has not been discussed as discordant redshift system.

Notes

– The position of the QSO (object 2) near NGC 5107 is very close to the minor axis of NGC 5107.

– There are some additional redshifts in NED for the objects further away from NGC 5107. Object 3 is in opposite side of NGC 5107 than object 2 and they are aligned across NGC 5107 nucleus. Object 2 is very close to NGC 5107 while object 3 is much further.

– There’s a good pair alignment across NGC 5107 containing objects 4 and 7. Redshift of object 7 is almost twice the redshift of object 4.

– Objects 4 and 5 have same redshift and same angular separation from NGC 5107.

– Objects 6, 7 and 8 have same redshift and their angular separation from NGC 5107 is also similar.


Figure 1. The objects with measured redshifts near NGC 5107. Size of the image is 15 x 15 arcmin. Image is from Digitized Sky Survey (POSS2/UKSTU Blue).

Objects and their data

NBR NAME TYPE REDSHIFT MAG SEPARATION
1 NGC 5107 SB(s)d? 0.003156 (946 km/s) 13.81 0
2 [HB89] 1319+388 QSO 0.955461 19.2 (g) 0.740
3 SDSS J132109.35+382733.1 galaxy 0.442012 20.4 (g) 5.578
4 2MASX J13214433+3826268 galaxy 0.238366 19.0 (g) 6.964
5 2MASX J13212161+3825189 galaxy 0.238114 18.8 (g) 6.970
6 SDSS J132056.64+382715.2 galaxy 0.426913 20.8 (g) 7.423
7 SDSS J132104.31+383855.0 galaxy 0.426460 21.2 (g) 7.759
8 SDSS J132051.31+382803.0 galaxy 0.426686 20.9 (g) 7.766

NED objects within 10′ from NHC 5107
SDSS image of the system.

References

Arp, 1981, ApJ, 250, 31, “Quasars near companion galaxies”

Bukhmastova, 2001, ARep, 45, 581, “Properties of Quasar-Galaxy Associations and Gravitational Mesolensing by Halo Objects”

Burbidge et al., 1990, ApJS, 74, 675, “Associations between quasi-stellar objects and galaxies”

Burbidge, 1996, A&A, 309, 9, “The reality of anomalous redshifts in the spectra of some QSOs and its implications”