Forming?
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by
GoldenRule
Is this rare? Why does it look like this, or what could cause it? Looks like the fibinachi spiral
Posted
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by
ElisabethB
moderator
Hi GolenRule and welcome to the Zoo
I'd classify this one as a very disturbed spiral galaxy, interacting with the one to the left (see the zoomed out view) . Nice #merger !
Happy hunting ! 😄
Posted
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by
zoob1172
in response to GoldenRule's comment.
There are thousands of objects in groups. There are 19 more objects north of this one.
There is a NED note about the object too.- 2000ApJS..131..413Z
Re:MCG +02-04-025
5.2.1. MCG +02-04-025
MCG +02-04-025=IRAS 01173+1405 is a spiral with an optical extension of
about 18" x 30" (Mirabel & Sanders 1988). In the DSS image there is a hint
of a bridge of material between the galaxy and a fainter galaxy only ~1'
to the east (Fig. 2). The interaction between the galaxies might be
responsible for the log(L_FIR_/L_sun_) = 11.27. Mirabel & Sanders (1988)
also note that the H I line profile is not the "horned" double peak of a
normal spiral but is a single peak more common to galaxies that have
suffered some interaction. They detected MCG +02-04-025 in H I in both
emission and absorption. From their detection they deduce an atomic gas
mass greater than 3.4 x 10^9^ M_sun_, most of which must be concentrated
near the core in order to provide a sufficient optical depth to explain
the absorption. Our observations show this galaxy to be marginally resolved
at 100 microns (Fig. 2), with a D_g_ = 19.5" and a D_e_ = 11". The galaxy
profile is slightly larger than the PSP, but better evidence comes from the
photometry. The entire IRAS flux is not recovered using the sum of
detectors 1-10, and the detectors 11-20 show little evidence for any
emission. This leaves the other side of the detector 1-10 arm of the array
(to the southeast) as the place that may have the missing IRAS flux.
Using the flux from the center detector 5, the exponential disk model
fit to our data gives an r_o_ ~ 6.5" when compared to the larger IRAS beam
measurement. This is close to but larger than the r_0_ ~ 5" derived using
the same exponential disk model with multibeam photometry at K
(Carico et al. 1990b). Using the size of 2 x r_o_ = 11", our 100 micron
flux, and a 60 micron flux scaled so that the S_60_/S_100_ ratio is the
same as the Soifer et al. (1989) fluxes, we derive a T_d_ = 44.6 and
{tau}100 = 2.1 x 10^-3^ from which A_V_ ~ 1.6. The A_V_ derived here
from the FIR fluxes and size is low considering the large gas column
density implied by Mirabel & Sanders (1988).
The possible extension at FIR wavelengths is interesting when compared
to the radio morphology. The estimated size of the emission region depends
on the size of the interferometric array. With a synthesized 6" beam
(1.49 GHz; CHSS) find a Gaussian size 2" x 2". With a smaller 0.25" beam
(8.44 GHz; CHYT) the size is only 1.2" x 0.8". Also, VLBI studies found an
extremely compact core with emission on 5, 10, and 50 mas scales (Lonsdale,
Smith, & Lonsdale 1993; Smith, Lonsdale, & Lonsdale 1998)
The radio studies argue quite convincingly that there is a compact
radio core that might even be small enough that it becomes difficult to
explain the luminosity with a starburst and its supernovae
(Smith et al. 1998). However, the fact that in each case the radio emission
was resolved, along with the possible extension in the FIR, argue that
while a central luminous radio core may exist (weak AGN or starburst), much
of the FIR flux originates on larger spatial scales. If one assumes that
the FIR flux is due to dust heated by a central compact source, a simple
spherically symmetric dust model (Barvainis 1987) suggests that this dust
might have a size ~19". This size assumes that the luminosity of the central
source in the UV matches the FIR luminosity and the dust at T_d_ = 45 has a
clear view of the core. For dust distributed in an optically thick disk,
this is unlikely. Thus, for this object, it can be concluded that while the
far-infrared emission is likely to be emitted in distributed sources, the
situation in principle energetically allows those sources to be heated by
a central source, whether AGN or compact starburst
Posted
- 2000ApJS..131..413Z
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by
ElisabethB
moderator
in response to zoob1172's comment.
Could you explain this in plain English and for the not-expert, please ?
Posted
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by
zoob1172
As of 2000 Eric C. Zink, Dan F. Lester, Greg Doppmann, and Paul M. Harvey Astronomy Department and McDonald Observatory, University of Texas, Austin, TX 78712
Posted
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by
ElisabethB
moderator
in response to zoob1172's comment.
Errmm, okay ! I was just asking you to put your previous post into something more accessible. This one does not help at all.
Posted