Updating to 4 01 m33
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.
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.
While we can rule out interstellar pressure as the major contributing factor, we are unable to disentangle the relative effects of metallicity and H velocity dispersion.
We find a reasonably featureless number density profile with galactocentric radius, and weak correlations between galactocentric radius and dust temperature/mass.
A system of seven spiral arms is pointed out by Ivanov & Kunchev (1985). (2004), (8) An, Terndrup & Pinsonneault (2007), (9) Freedman et al. Studying the kinematics of such a galaxy will provide a better understanding of the contribution of DM and of the best functional form describing its distribution.
= 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.
= 69°02'32".30 Located 96" east and 83" north of the center of M81 (Discovery image) Mag 19.8:4/14, Type unknown (References: CBAT TOCP) For more information in Extra galactic novae, look at the Extra Galactic Nova links on the links page.
2010; Inoue & Saitoh 2011; Ogiya & Mori 2011; Pontzen & Governato 2012; Teyssier et al. Several studies of the kinematics of M33 exist (e.g. However, they argue that these values could even be lower if taking into account the instrumental corrections. The precise determination of the rising parts of RCs with high-resolution data and a better estimate of the M/L ratio for the stellar disc could define more accurately the shape of its DM halo.
Corbelli & Salucci 2000; Corbelli 2003; Putman et al. The mass-to-light ratio (M/L) is an important parameter in the determination of the DM halo shape. High-resolution optical observations of a nearby galaxy such as M33 is complex in view of the large size of the galaxy compared to the small field of view (FOV) of high-resolution integral field spectroscopic instruments. High-resolution Hα RCs give a more accurate determination of the kinematical parameters for the derivation of the RCs and subsequently a more accurate determination of the mass model parameters.