Maffei 1: a New Massive Member of the Local Group?

Spinrad, Hyron; Sargent, W. L. W.; Oke, J. B.; Neugebauer, G.; Landau, R.; King, Ivan R.; Gunn, James E.; Garmire, Gordon; Dieter, Nannielou H.

doi:10.1086/180660

Cited by 23 publications

(27 citation statements)

References 6 publications

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“…Realizing that adequate photometry was lacking, Buta & McCall (1999) acquired images of Maffei 1 in B, V, and Cousins I, using a CCD camera attached to the Burrell Schmidt telescope at Kitt Peak. After foreground stars were carefully removed, the apparent V magnitude was found to be 11:14 AE 0:06 mag, confirming the earlier results of Spinrad et al (1971) and Buta & McCall (1983). At the lower distance of Buta & McCall (1983), the absolute magnitude (M V ¼ À20:6) would make Maffei 1 an intermediate elliptical by the standards of galaxies in the Virgo Cluster.…”

Section: Introductionsupporting

confidence: 84%

“…Luppino & Tonry (1993) also applied the D n -relation to arrive at an independent estimate of distance. The result, 4:2 AE 1:1 Mpc, agreed with that from surface brightness fluctuations, but the observational ingredients were highly uncertain, being founded on their surface photometry in K 0 (to only 90 00 , i.e., 30% of D n ), an average BÀK color for elliptical galaxies, and the velocity dispersion of Spinrad et al (1971). The method is reexamined in x 6 using modern data.…”

Section: Introductionmentioning

confidence: 66%

“…The subsequent flurry of research activity led to its tentative identification as an elliptical galaxy (Spinrad et al 1971), later confirmed by Buta & McCall (1983 and Luppino & Tonry (1993). By comparing the nuclear spectrum with spectra of the spheroid of M31 and giant ellipticals like NGC 3379, Spinrad et al (1971) estimated A V to be 5:2 AE 0:2 mag. Upon visual inspection of a photographic spectrum, they concluded that the velocity dispersion was '' not less than 150 km sec À1 or greater than 250 km sec À1 ''; a value of 200 km s À1 was adopted.…”

Section: Introductionmentioning

confidence: 92%

“…Subsequent estimates of extinction based on studies of foreground stars indicated that the result of Spinrad et al (1971) might be a magnitude or more too high (see Buta & McCall 1983). Buta & McCall (1983) added two new measurements.…”

Section: Introductionmentioning

confidence: 99%

“…Through a gross extrapolation of the aperture growth curve, the apparent visual magnitude was determined to be 11.4 mag. Combining the velocity dispersion estimated by Spinrad et al (1971) with the measurements of extinction and brightness, a distance of 2:1 þ1:3 À0:8 Mpc was derived from the relationship between luminosity and central velocity dispersion observed in V for elliptical galaxies, as defined by de Vaucouleurs & Olson (1982). Thus, the galaxy no longer appeared to be in the Local Group, but instead in a collection of galaxies known at the time as the Ursa Major-Camelopardalis Cloud (de Vaucouleurs 1975).…”

Section: Introductionmentioning

confidence: 99%

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The Extinction and Distance of Maffei 1

Fingerhut

McCall

Robertis

et al. 2003

ApJ

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We have obtained low-and high-resolution spectra of the core of the highly reddened elliptical galaxy Maffei 1. From these data, we have obtained the first measurement of the Mg 2 index and have measured the velocity dispersion and radial velocity with improved accuracy. To evaluate the extinction, a correlation between the Mg 2 index and effective VÀI color has been established for elliptical galaxies. Using a new method for correcting for effective wavelength shifts, the VÀI color excess reveals that the optical depth of Galactic dust at 1 lm is 1:69 AE 0:07. Thus, A V ¼ 4:67 AE 0:19 mag, which is lower by 0.4 mag than previously thought. To establish the distance, the fundamental plane for elliptical galaxies has been constructed in I. The velocity dispersion of Maffei 1, measured to be 186:8 AE 7:4 km s À1 , in combination with modern widefield photometry in I, leads to a distance of 2:92 AE 0:37 Mpc. The D n -relation, which is independently calibrated, gives 3:08 AE 0:85 and 3:23 AE 0:67 Mpc from photometry in B and K 0 , respectively. The weighted mean of the three estimates is 3:01 AE 0:30 Mpc, which is lower than distances judged with reference to M32 and the bulge of M31 from the brightest stars seen at K 0 . Since the luminosity of asymptotic giant branch stars at K 0 is strongly dependent on age, the lower distance suggests that the last epoch of star formation in Maffei 1 occurred farther in the past than in these other systems. The distance and luminosity make Maffei 1 the nearest giant elliptical galaxy. In the absence of extinction, the galaxy would be among the brightest in the sky and would have an apparent size 2 3 that of the full Moon. The radial velocity of Maffei 1 is +66:4 AE 5:0 km s À1 , significantly higher than the accepted value of À10 km s À1 . The Hubble distance corresponding to the mean velocity of Maffei 1, Maffei 2, and IC 342 is 3.5 Mpc. Thus, it is unlikely that Maffei 1 has had any influence on Local Group dynamics.

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Section: Introductionsupporting

confidence: 84%

Section: Introductionmentioning

confidence: 66%

Section: Introductionmentioning

confidence: 92%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Extinction and Distance of Maffei 1

Fingerhut

McCall

Robertis

et al. 2003

ApJ

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A Catalogue of Galaxies within 10 MPC

1979

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A catalogue is given of the 179 known galaxies within 10 Mpc. The inclusion of a galaxy depends on its redshift (vo 5 500 km s-l) or, in the case of 7 dwarf galaxies, on the fact that their distances are known to be small. The catalogue contains in addition 52 more distant galaxies with vo 5 500 km s-l: 50 are bona fide Virgo cluster members and 2 are members of the Leo group. Positions, types, absorption-corrected luminosities, and velocities are given for the catalogue galaxies. The catalogue is believed t o be nearly complete for galaxies brighter than --18Lf5. but i t contains also many considerably fainter galaxies. The galaxies within 10 Mpc form the Local Group with 28 members and seven additional groups with a total of 92 known members. 59 galaxies (33%) do not seem to belong to any group.Der Katalog e n t M t die 179 bekannten Galaxien innerhalb 10 Mpc. Die Aufnahme einer Galrtvie hangt von ihrer Rotverschiebung (vo 5 500 km s-9 oder im Falle von 7 Zwerggalaxien von deren bekannter geringer Entfernung ab. Der Katalog enthiilt weiterhin 52 entferntere Galaxien mit vo 5 500 km s-l; davon sind 50 bona fide Mitglieder des Virgohaufens und z gehoren zur Leo-Gruppe. Position, Typ, wegen Absorption korrigierte Helligkeit und Geschwindigkeit sind far jede Galaxie gegeben. Man darf annehmen, daD der Katalog ftir Galaxien heller als -18.5ter GrdBe nahezu komplett ist, jedoch enthalt er auch viele wesentlich schwachere Galaxien. Die Galaxien innerhalb 10 Mpc bilden die lokale Gruppe mit 28 Mitgliedern und 7 weitere Gruppen mit einer Gesamtzahl von 92 bekannten Mitgliedern. 59 Galaxien (33%) scheinen zu keiner Gruppe zu gehbren.The present catalogue represents the first attempt at compiling a distance-limited sample of galaxies. It compiles all galaxies known within 10 Mpc.Lacking accurate distance information for most galaxies recession velocities v, (corrected for solar motion) are actually used as selection criterium instead of distances. Hence the catalogue contains all galaxies with v, 5 500 km s-l (H, = 50 km s-l Mpc-l).The substitution of distances by recession velocities is justified in view of the small peculiar velocities of galaxies. The mean radial component of the peculiar motions of nearby field and group galaxies is 5 50 km s-l (TULLY and FISHER, 1978; TAMMANN and KRAAN, 1978), -therefore the substitution of distances by recession velocities introduces a mean distance error of only 5 10 percent at the catalogue limit.There is one important exception, where the assumption of small peculiar motions does not apply: Virgo cluster members, which populate the low-velocity tail of the cluster velocity distribution ((vo)virp0 = 1050 km s-l, uvirgo = 690 km s-l; cf. SANDAGE and TAMMANN, 1978), do enter the present catalogue, although their distance is, of course, much larger than 10 Mpc. 50 galaxies in the present catalogue can be identified as almost certain lowvelocity Virgo cluster members, because they are densely clumped within a circle around the cluster center with a radius of only 4?8! These 50 Virgo c...

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A Quarter Century of Listening Pleasure — 25 Years’ Research with the WSRT

Strom¹

1996

The Westerbork Observatory, Continuing Adventure in Radio Astronomy

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Maffei 1: a New Massive Member of the Local Group?

Abstract: An extensive collection of observational data is presented which indicates that the recently discovered infrared object Maffei 1 is a highly reddened giant elliptical galaxy at a distance of about 1 Mpc, and thus is probably a new massive member of the Local Group.

Cited by 23 publications

References 6 publications

The Extinction and Distance of Maffei 1

The Extinction and Distance of Maffei 1

A Catalogue of Galaxies within 10 MPC

A Quarter Century of Listening Pleasure — 25 Years’ Research with the WSRT

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