Kapteyn Institute Preprints (2002)
Kapteyn Institute Preprint Service.
Preprints of the Kapteyn Institute.
Paper copies can be ordered at:
Kapteyn Institute
P.O. Box 800
9700 AV Groningen
The Netherlands
All the preprints are compressed using gzip.
2002 Preprints
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astro-ph/0212467 Discs
in early-type lensing galaxies: effects on magnification ratios and
measurements of $H_0$. Ole Moeller, Paul Hewett, A.W. Blain
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astro-ph/0212293 Clusters
of galaxies with modified Newtonian dynamics (MOND). R.H. Sanders
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astro-ph/0211637 A
deep search for 21cm absorption in high redshift damped Lyman-$\alpha$ systems.
Nissim Kanekar, Jayaram N. Chengalur
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astro-ph/0211451 Rapid
Variability and Annual Cycles in the Characteristic Time-scale of the
Scintillating Source PKS 1257-326. H.E. Bignall, D.L. Jauncey, J.E.J.
Lovell, A.K. Tziournis, L. Kedziora-Chudczer, J.-P. Macquart, S.J. Tingay,
D.P. Rayner, R.W. Clay
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astro-ph/0210504 B0850+054:
a new gravitational lens system from CLASS. A.D. Biggs, D. Rusin, I.W.A.
Browne, A.G. de Bruyn, N.J. Jackson, L.V.E. Koopmans, J.P. McKean, S.T. Myers,
R.D. Blandford, K.-H. Chae, C.D. Fassnacht, M.A. Norbury, T.J. Pearson, P.M.
Phillips, A.C.S. Readhead
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astro-ph/0210234 CLASS
B0445+123: a new two-image gravitational lens system. M.K. Argo, N.J.
Jackson, I.W.A. Browne, T. York, J.P. McKean, A.D. Biggs, R.D. Blandford, A.G.
de Bruyn, K.H. Chae, C.D. Fassnacht, L.V.E. Koopmans, D.R. Marlow, S.T. Myers,
M. Norbury, T.J. Pearson, P.M. Phillips, A.C.S. Readhead, D. Rusin, P.N.
Wilkinson
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astro-ph/0210031 Rapidly
Evolving Circularly Polarized Emission during the 1994 Outburst of GRO
J1665-40. J.-P. Macquart, K. Wu, R.J. Sault, D.C. Hannikainen
Preprint
337 MOND rotation curves for spiral galaxies with Cepheid-based
distances. Roelof Bottema, Jose L.G. Pestana, Barry Rothberg, Robert H.
Sanders
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astro-ph/0207116 HST/WFPC2
proper motions in two bulge fields: kinematics and stellar population of the
Galactic bulge. Konrad Kuijken, R. Michael Rich
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astro-ph/0207112 Neutral
Hydrogen and Optical Observations of Edge-on Galaxies: Hunting for Warps.
I. Garcia-Ruiz, R. Sancisi, K. Kuijken
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astro-ph/0207041 Discovery
of a Group of Star-Forming Dwarf Galaxies in Abell 1367. Shoko Sakai,
Robert Kennicutt, J.M. van der Hulst, Chris Moss
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astro-ph/0206427 Froth
across the Universe Dynamics and Stochastic Geometry of the Cosmic Foam.
Rien van de Weygaert
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astro-ph/0206420 High
Resolution 4.7 um Keck/NIRSPEC Spectra of Protostars. II: Detection of the
13CO Isotope in Icy Grain Mantles. A.C.A. Boogert, G.A. Blake, A.G.G.M.
Tielens
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astro-ph/0206381 Report
to Anaximander: A Dialogue on the Origin of the Cosmos in the Cradle of
Western Civilization. Rien van de Weygaert
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astro-ph/0206366 The
Cosmic Foam: Stochastic Geometry and Spatial Clustering Across the Universe.
Rien van de Weygaert
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astro-ph/0205450 Automatic
Observation Rendering (AMORE) I. On a synthetic stellar population's
colour-magnitude diagram. Y.K. Ng, E. Brogt, C. Chiosi, G. Bertelli
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astro-ph/0205254 The
stellar content, metallicity and ionization structure of HII regions. N.L.
Martin-Hernandez, R. Vermeij, A.G.G.M. Tielens, J.M. van der Hulst, E. Peeters
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astro-ph/0205196 The
Radio Properties of Composite LINER/HII Galaxies. Mercedes E. Filho, Peter
D. Barthel, Luis C. Ho
astro-ph/0204521 Modified
Newtonian Dynamics as an Alternative to Dark Matter. Robert H. Sanders,
Stacy S. McGaugh
- Preprint 336 Dark and luminous matter in the NGC 3992
group of galaxies. II. The dwarf companions UGC 6923, UGC 6940, UGC 6969, and
the Tully-Fisher relation. Roelof Bottema
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Preprint 335 Dark and luminous matter in the NGC 3992
group of galaxies. I. The large barred spiral NGC 3992. Roelof Bottema
and Marc A.W. Verheijen
astro-ph/0204093 Microarcsecond
Radio Imaging using Earth Orbit Synthesis. J.-P. Macquart, D.L. Jauncy
astro-ph/0203405 Deep
H I Survey of the Spiral Galaxy NGC 2403. Filippo Fraternali, Gustaaf van
Moorsel, Renzo Sancisi, Tom Oosterloo
astro-ph/0201484 Automating
the Synthetic Field Method:Application to Sextans A.Benne W. Holwerda,
Ronald J. Allen, Pieter C. van der Kruit
astro-ph/0201141 Detection
of a Thick Disk in the edge-on Low Surface Brightness Galaxy ESO 342-G017: I.
VLT Photometry in V and R Bands. Mark J. Neeser, Penny D. Sackett, Guido
de Marchi, Francesco Paresce
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Roelof Bottema, Jose L.G. Pestana, Barry Rothberg, Robert H. Sanders
Preprint no. 337
Accepted for publication in Astronomy and Astrophysics.
Abstract
Rotation curves for four spiral galaxies with recently determined
Cepheid-based distances are reconsidered in terms of modified Newtonian
dynamics (MOND). For two of the objects, NGC 2403 and NGC 7331, the
rotation curves predicted by MOND are compatible with the observed curves
when these galaxies are taken to be at the Cepheid distance. For NGC 3198,
the largest distance for which reasonable agreement is obtained is 10%
smaller than the Cepheid-based distance; i.e., MOND clearly prefers a smaller
distance. This conclusion is unaltered when new near-infrared photometry of
NGC 3198 is taken as the tracer of the stellar mass distribution. For the
large Sc spiral, NGC 2841, MOND requires a distance which is at least 20%
larger than the Cepheid-based distance. However, the discrepancy of the
Tully-Fisher and SNIa distances with the Cepheid determination casts some
doubt upon the Cepheid method in this case.
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Roelof Bottema
Preprint no. 336
Accepted for publication in Astronomy and Astrophysics.
Abstract
Detailed neutral hydrogen observations have been obtained of the large barred
spiral galaxy NGC 3992 and its three small companion spiral galaxies, UGC
6923, UGC 6940, and UGC 6969. Contrary to the large galaxy, for the companions
the HI distribution ends quite abruptly at the optical edges. Velocity fields
have been constructed from which rotation curves have been derived. Assuming a
reasonable M/L ratio, a decomposition of these rotation curves generates
nearly equal dark matter halos. When comparing the position-velocity diagrams
of the two brightest galaxies, UGC 6923 and UGC 6969, it is obvious that the
rotation curve of the latter has a shape closer to solid body than the former,
yet the same maximum rotational level is reached. This is likely generated by
the equal dark matter halos in combination with UGC 6923 being a factor five
more luminous than UGC 6969 and so its luminous matter gives a higher
contribution to the rotation in the inner regions. An NFW-CDMLambda dark halo
is consistent with the observed rotation curve of UGC 6923 but not consistent
with the rotation curve of UGC 6969. If the NGC 3992 group is part of the Ursa
Major cluster, then the I-band M/L ratio of NGC 3992 has to be at least 1.35
times as large as that of the average spiral galaxy in the cluster. On the
other hand, equal M/L ratios can be achieved when the NGC 3992 group is placed
more than 3 Mpc behind the cluster. Both possibilities can explain why NGC
3992 appears to be 0.43 magnitudes too faint for its rotation..
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Roelof Bottema and Marc A.W. Verheijen
Preprint no. 335
Accepted for publication in Astronomy and Astrophysics.
Abstract
Detailed neutral hydrogen observations have been obtained of the large barred
spiral galaxy NGC 3992 and its three small companion galaxies, UGC 6923, UGC
6940, and UGC 6969. For the main galaxy, the HI distribution is regular with a
low level radial extension outside the stellar disc. However, at exactly the
region of the bar, there is a pronounced central HI hole in the gas
distribution. Likely gas has been transported inwards by the bar and because
of the emptyness of the hole no large accretion events can have happened in
recent galactic times. The gas kinematics is very regular and it is
demonstrated that the influence of the bar potential on the velocity field is
negligible. A precise and extended rotation curve has been derived showing
some distinct features which can be explained by the non-exponential radial
light distribution of NGC 3992. The decomposition of the rotation curve gives
a slight preference for a sub maximal disc, though a range of disc
contributions, up to a maximum disc situation fits nearly equally well. For
such a maximum disc contribution, which might be expected in order to generate
and maintain the bar, the required mass-to-light ratio is large but not
exceptional.