Updating to 4 01 m33
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.Fukushige & Makino 1997; Navarro, Frenk & White 1997; Moore et al. Phenomena such as stellar feedbacks, galactic winds or massive clumps are not often well handled and reproduced (Goerdt et al. Valcheva image) Mag 19.6:7/10 (16.7:7/8), Type He/N (References: ATEL 5092, 5099, 5123, 5145, 5257, 12915, 12943, TNS, ZTF observations, CBAT TOCP) AT2019kli (= ASASSN-19qv), TNS discovered 2019/07/04.290 by All Sky Automated Survey for Super Novae (ASAS-SN) Found in SMC at R. = 41°14'12".5 Located 127".5 east and 116".0 south of the center of M31 (Kamil Hornoch image) (A. = -73°46'22".73 Located 3040".5 east and 3399".8 south of the center of SMC (Joseph Brimacombe image) Mag 14.2:7/4, Type Nova (References: ATEL 12907, 12917, 12938, 12990) AT2019iby (= ZTF19aawtdov) (= LPV J013232.49 303521.8), TNS discovered 2019/06/20.445 by Zwicky Transient Facility (ZTF) Found in M33 at R. (= PNV J00424173 4117537) (= PNV J00424176 4117534), ATEL 12895 discovered 2019/06/27.065 by Kamil Hornoch and Peter Kusnirak Found in M31 at R. ) (= PNV J00455384 4217028) (= ATLAS19ocz), CBAT TOCP discovered 2019/06/25.626 by Koichi Itagaki Found in M31 at R. (= PNV J09554664 6902473), ATEL 12859 discovered 2019/06/09.875 by Kamil Hornoch et al. = 40°42'33".10 Located 0".0 east and 0".0 north of the center of M31 (Discovery image) (Emmanuel Conseil image) (Emmanuel Conseil image) Mag 18.0:5/6 (17.2:4/25), Type unknown (References: VSnet observations) Nova M31 2019-04a? = 41°13'57".70 Located 116".9 west and 130".8 south of the center of M31 (Discovery image) Mag 17.3:4/16, Type unknown (References: CBAT TOCP) AT2019dlz (= XM10MZ) (= PNV J09555100 6902323), TNS discovered 2019/04/14.669 by Xingming Observatory Sky Survey (XOSS) Found in M81 at R. Look at the updates page for a list of the most recent changes and additions to these pages.
CBET has a naming convention now for novae in M31 (now extended to Novae in M33 and M81). = 41°13'42".30 Located 68".6 west and 146".3 south of the center of M31 (Discovery image) (Hornoch image) Mag 16.2:8/5, Type Fe II (References: ATEL 12999, TNS, ATEL 12989) AT2019lvm (= Bra TS-Bra TS-T1-003) (= TCP J05293666-7009566), TNS discovered 2019/07/27.349 by Bra TS Found in LMC at R.
As part of a long-term project to revisit the kinematics and dynamics of the large disc galaxies of the Local Group, we present the first deep, wide-field (∼42 arcmin × 56 arcmin) 3D-spectroscopic survey of the ionized gas disc of Messier 33.
Fabry–Perot interferometry has been used to map its Hα distribution and kinematics at unprecedented angular resolution (≲3 arcsec) and resolving power (∼12 600), with the 1.6 m telescope at the Observatoire du Mont Mégantic.
In the optical bands, it could be considered as a flocculent spiral galaxy, but UV and IR observations show more prominent arms. The optical parameters of M33 are given in Table 1. It is the mean distance estimated by using resolved sources techniques such as Cepheids, Planetary Nebulae Luminosity Function (PNLF) and Tip of the Red Giant Branch (TRGB). Still today, the cusp–core problem remains as one compares observations to predictions, especially for dwarf systems and this, despite the numerous studies on the DM distribution in galaxies in the last 30 years.
The M33 profile presents a small bulge-like component in the IR bands. The optical disc of M33 has a scalelength of ∼9.2 arcmin (2.25 kpc) in the References: (1) Mc Connachie et al. (2008), (3) Galleti, Bellazzini & Ferraro (2004), (4) Magrini et al. While, on large scales, -body cosmological simulations reproduce well the observations, it is more problematic at galaxy scales.