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The ionized gas distribution follows a complex, large-scale spiral structure, unsurprisingly coincident with the already-known spiral structures of the neutral and molecular gas discs.
The kinematical analysis of the velocity field shows that the rotation centre of the Hα disc is distant from the photometric centre by ∼168 pc (sky-projected distance) and that the kinematical major-axis position angle and disc inclination are in excellent agreement with photometric values.
The Hα rotation curve agrees very well with the H , which is at the low end of velocity dispersions of nearby star-forming galactic discs.
A strong relation is also found between the Hα velocity dispersion and the Hα intensity.
However, it is the rising inner part of the RCs that constrains the parameters of the mass models (see e.g. The objective of this project is to perform a new mass distribution model of Messier 33 (M33), combining high-sensitivity Hα and H interferometric data. (2004), (8) An, Terndrup & Pinsonneault (2007), (9) Freedman et al. 2009), confirms that there were many mergers and interactions between them.
In particular, this article presents the first Hα survey devoted to the large-scale distribution and kinematics of the M33 ionized gas disc. The discovery of dwarf galaxies around the Milky Way and M31 and the tidal streams between M31 and M33 (PAn DAS) confirm our ideas about galaxy formation.
= 41°23'58".40 Located 251".9 west and 469".9 north of the center of M31 (Discovery image) Mag 16.7:5/24, Type unknown (References: CBAT TOCP) Nova M31 2019-04b? = 41°16'26".30 Located 29".1 west and 17".8 north of the center of M31 (Discovery image) Mag 16.6:4/26, Type unknown (References: CBAT TOCP) AT2019ebb, TNS discovered 2019/04/25.215 by Emmanuel Conseil Found in M31 at R. (= PNV J00423396 4113577), ATEL 12666 discovered 2019/04/16.121 by Kamil Hornoch and Hana Kucakova Found in M31 at R.
These clouds are reasonably consistent with Larson’s scaling relationships, and many of our sources are co-spatial with earlier CO studies.
Massive clouds are identified at large galactocentric radius, unlike in these earlier studies, perhaps indicating a population of CO-dark gas dominated clouds at these larger distances.
Much of this data comes from CBET Circulars and occasionally more data will be provided on IAU's Astronomical Headlines page. = 41°19'19".40 Located 186".8 east and 190".9 north of the center of M31 (Discovery image) Mag 17.3:7/11 (15.9:5/8), Type unknown (References: CBAT TOCP) Nova M31 2019-07b? = 41°06'04".00 Located 501".0 east and 605".0 south of the center of M31 Mag 17.8:7/2, Type unknown AT2019lcd (= Nova M31 2013-05b?
CBET now has an M31 novae page, M33 novae page, and an M81 novae page. = 41°49'39".93 Located 943".8 west and 2011".4 north of the center of M31 Mag 16.9:7/13, Type Nova (References: ATEL 12953, ZTF observations) Nova M31 2019-07c? (= PNV J00432865 4106040), CBAT TOCP discovered 2019/07/02.678 by Koichi Itagaki Found in M31 at R. ) (= ZTF19abfqlzi) (= PNV J00425563 4114125) (= M31N 1960-12a), ATEL 5091 discovered 2013/05/29.033 by F.
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Its bulge and nucleus are the subject of numerous studies (e.g. The NFW profile, derived from those simulations, predicts a cuspy distribution in the central parts of the DM haloes (e.g. 2013), while observations especially of dwarf systems show more a core distribution (Oh et al. Those results can be explained by the gravitational potential related to the gas in those simulations, since the gas, which is important in the inner parts, is not accurately introduced in those simulations.