Upper limit to the neutral hydrogen content of the elliptical galaxy NGC 4472 .

1974 ◽  
Vol 79 ◽  
pp. 667 ◽  
Author(s):  
G. R. Knapp ◽  
F. J. Kerr
Keyword(s):  
Hydrogen Content ◽  
Elliptical Galaxy ◽  
Neutral Hydrogen ◽  
Upper Limit

scholarly journals Sensitive Search for HI in E and SO galaxies

1983 ◽  
Vol 100 ◽  
pp. 305-306
Author(s):  
Norbert Thonnard
Keyword(s):  
Neutral Hydrogen ◽  
Optical Image ◽  
Type I ◽  
Hydrogen Line ◽  
Upper Limit

Do elliptical and SO galaxies in which type I supernovae (SNI) were detected contain more gas than those without SNI detections? Thirteen E and SO galaxies in the Virgo and Pegasus I clusters, seven with SNI detections and six without, were mapped well beyond the optical image at the 21-cm neutral hydrogen line. No HI was detected. In Virgo, the upper limit to MMI/LB is between 0.0005 and 0.0024.

scholarly journals The Ring of HI in LEO: Probing the Mass Distribution in a Galaxy Group

1987 ◽  
Vol 117 ◽  
pp. 116-116
Author(s):  
Stephen E. Schneider ◽  
Edwin E. Salpeter ◽  
Yervant Terzian
Keyword(s):  
Mass Distribution ◽  
Elliptical Galaxy ◽  
Neutral Hydrogen ◽  
Ring Structure ◽  
Intergalactic Gas ◽  
Large Ring ◽  
Eccentric Ring

The intergalactic neutral hydrogen in the M96 group (Schneider et al. 1983) provides an unusual probe of the detailed mass distribution in a group of galaxies. Previous observations (Schneider 1985) tentatively suggested the existence of a large ring structure to the gas. Sensitive new observations made at Arecibo confirm that the intergalactic gas forms a 200 kpc diameter eccentric ring around the two central galaxies in the group, the giant elliptical galaxy NGC 3379 (M105) and the lenticular NGC 3384.

scholarly journals Hydrogen Content of Young Stellar Clusters. I. Methods of Observation and Reduction

1973 ◽  
Vol 26 (6) ◽  
pp. 829 ◽  
Author(s):  
HM Tovmassian
Keyword(s):  
Radio Telescope ◽  
Hydrogen Content ◽  
Data Reduction ◽  
Neutral Hydrogen ◽  
Hydrogen Gas ◽  
Continuum Emission ◽  
Stellar Clusters ◽  
Hydrogen Line ◽  
Galactic Clusters

Observations of 16 open galactic clusters in their continuum emission and at the neutral hydrogen line have been made with the Parkes 64 m radio telescope in an attempt to determine the total amount of hydrogen gas associated with them. In this, the first of a series of five papers, the observing procedure and the method of data reduction are described.

scholarly journals The Distribution and Kinematics of Neutral Hydrogen in NGC 807

1987 ◽  
Vol 127 ◽  
pp. 423-424
Author(s):  
L. L. Dressel
Keyword(s):  
Elliptical Galaxy ◽  
Line Emission ◽  
Neutral Hydrogen ◽  
Minor Axis ◽  
Dynamical Equilibrium ◽  
Arecibo Observatory

I have detected 21 cm line emission from neutral hydrogen in the giant elliptical galaxy NGC 807 at Arecibo Observatory, and I have mapped this emission with the VLA. Unlike the active and dwarf ellipticals that have been mapped thus far, NGC 807 has a fairly regular disk of gas rotating about the apparent optical minor axis. Combined with observations of active ellipticals, this observation suggests that two classes of HI-rich ellipticals may exist: ellipticals which have accreted gas and become active recently, and quiescent ellipticals which have either produced gas internally or accreted it so long ago that it has reached dynamical equilibrium.

scholarly journals The Dark Massive Halo in the Elliptical Galaxy NGC 5266

1995 ◽  
Vol 164 ◽  
pp. 446-446
Author(s):  
A. Pizzella ◽  
R. Morganti ◽  
M.E. Sadler ◽  
F. Bertola
Keyword(s):  
Spiral Galaxies ◽  
Elliptical Galaxy ◽  
Neutral Hydrogen ◽  
Major Axis ◽  
Minor Axis ◽  
Representative Point ◽  
Dust Lane ◽  
The Galaxy ◽  
Central Regions ◽  
Parallel Behaviour

Recent observations with the Australia Telescope reveal that the elliptical galaxy NGC 5266 has a disk like structure of neutral hydrogen extending as far as almost 10 Re which approximatively lies along the galaxy's major axis, at 65° apart from the inner minor–axis dust lane (Varnas et al 1987). From the present data is not clear whether the HI structure and the dust lane are two distinct disks or a single warped structure. The regularity of the velocity field of the HI structure allow us to use it as a probe of the potential of NGC 5266. The velocity curve along the major axis is flat till the last measured point (rmax ~ 10′) at Vrot = 200km/s. Assuming that the gas in moving in circular orbits, we can derive the mass of the galaxy inside to this radius. The mass–to–light ratio M/LB rises from about 3 in the central regions to 12 at 9 Re (D = 57.6 Mpc), thus indicating that NGC 5266 is embedded in a dark massive halo. Moreover the representative point (cumulative M/LB within the last measured point) of NGC 5266 in the diagram log(M/LB) – log(Re) falls well within the region characteristic of spiral galaxies (Figure 2, Bertola et al. 1993), as do ellipticals previously studied in HI, thus reinforcing the suggestion (Bertola et al. 1993) of a parallel behaviour of the dark matter in elliptical and spiral galaxies.

The neutral hydrogen content of early type disk galaxies

1991 ◽  
Vol 102 ◽  
pp. 572 ◽  
Author(s):  
J. Eder ◽  
R. Giovanelli ◽  
M. P. Haynes
Keyword(s):  
Hydrogen Content ◽  
Neutral Hydrogen ◽  
Disk Galaxies ◽  
Early Type

scholarly journals Measuring the distance to the black hole candidate X-ray binary MAXI J1348–630 using H i absorption

2020 ◽  
Vol 501 (1) ◽  
pp. L60-L64
Author(s):  
J Chauhan ◽  
J C A Miller-Jones ◽  
W Raja ◽  
J R Allison ◽  
P F L Jacob ◽  
...  
Keyword(s):  
Black Hole ◽  
Neutral Hydrogen ◽  
Tangent Point ◽  
X Ray ◽  
Black Hole Candidate ◽  
Upper Limit ◽  
Local Standard ◽  
Point Distance ◽  
Spectral State ◽  
Local Standard Of Rest

ABSTRACT We present neutral hydrogen (H i) absorption spectra of the black hole candidate X-ray binary (XRB) MAXI J1348–630 using the Australian Square Kilometre Array Pathfinder (ASKAP) and MeerKAT. The ASKAP H i spectrum shows a maximum negative radial velocity (with respect to the local standard of rest) of −31 ± 4 km s−1 for MAXI J1348–630, as compared to −50 ± 4 km s−1 for a stacked spectrum of several nearby extragalactic sources. This implies a most probable distance of $2.2^{+0.5}_{-0.6}$ kpc for MAXI J1348–630, and a strong upper limit of the tangent point distance at 5.3 ± 0.1 kpc. Our preferred distance implies that MAXI J1348–630 reached 17 ± 10  per cent of the Eddington luminosity at the peak of its outburst, and that the source transited from the soft to the hard X-ray spectral state at 2.5 ± 1.5  per cent of the Eddington luminosity. The MeerKAT H i spectrum of MAXI J1348–630 (obtained from the older, low-resolution 4k mode) is consistent with the re-binned ASKAP spectrum, highlighting the potential of the eventual capabilities of MeerKAT for XRB spectral line studies.

scholarly journals A Neutral Hydrogen Cloud in the Vicinity of the Elliptical Galaxy NGC 4318

1987 ◽  
Vol 115 ◽  
pp. 634-635
Author(s):  
L. Bottinelli ◽  
D. Fraix-Burnet ◽  
L. Gouguenheim
Keyword(s):  
Optical Properties ◽  
Radial Velocity ◽  
Elliptical Galaxy ◽  
Neutral Hydrogen ◽  
Morphological Type ◽  
Virgo Cluster ◽  
List Type ◽  
Type Number

NGC 4318, in the Virgo Cluster, has the following optical properties: —morphological type: E (Nilson, 1973)—BoT magnitude : 13.8 (Nilson, 1973)—photometric axis : 0.8′ × 0.6′ (Nilson, 1973)—heliocentric radial velocity: −300 km s−1 (Arakelian et al., 1975)1247± 15 km s (Tonry, 1981)1215 km s−1 (Huchra et al., 1983)

scholarly journals Hoag's object: the quintessential ring galaxy

2012 ◽  
Vol 10 (H16) ◽  
pp. 368-368
Author(s):  
Noah Brosch ◽  
Ido Finkelman ◽  
Alexei Moiseev
Keyword(s):  
Star Formation ◽  
Elliptical Galaxy ◽  
Neutral Hydrogen ◽  
Perfect Ring ◽  
Large Disk ◽  
Low Level ◽  
The Core ◽  
Event Triggered

AbstractWe present new observations of Hoag's Object, known as “the most perfect ring galaxy,“ that show that a preferred explanation for this object is (a) the formation of a triaxial elliptical galaxy some 10 Gyr ago, (b) the accretion of a large disk of neutral hydrogen at about the same time, (c) low-level star formation in the HI disk for all the time since that event triggered by the triaxial potential of the core.

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