Educação matemática pela arte
Gusmão, Lucimar Donizete
2013-08-28
Search results
23 records were found.
Comment: 8 pages, 8 figures, to be published in PASJ. Also available at
http://www-cr.scphys.kyoto-u.ac.jp/member/jun/job/ (with high-resolution
images)
Comment: A version with higher resolution figures is available from
http://www.a.phys.nagoya-u.ac.jp/~naoko/research/apjl2009/fur09_rev_highreso.pdf
Comment: 11 pages, 8 figures. Accepted for publication in A&A
Comment: Accepted by ApJ, 35pages including 14 figures
Comment: 17 pages, 13 figures, to appear in Protostars and Planets V. A full
color version with higher resolution figures is available at
http://astron.berkeley.edu/~blitz/PP5/ms.pdf
Comment: 24 pages, 16 figures, accepted by ApJ. A version with nice figures is
available at http://celestial.berkeley.edu/spitzer/publications/
We present new FIR maps of the SMC at 24, 70, and 160 μm obtained as part of the Spitzer Survey of the Small Magellanic Cloud (S^(3)MC). These maps cover most of the star formation in the SMC bar and wing. We combine our maps with literature data to derive the dust mass surface density across the SMC. We find a total dust mass of M_(dust) = 3 × 10^5 M_☉, implying a dust-to-hydrogen ratio over the region studied of log_(10)(D/H) = -2.86, or 1 : 700, which includes H_2. Assuming the dust to trace the total gas column, we derive H_2 surface densities across the SMC. We find a total H_2 mass M_(H_2) = 3.2 × 10^7 M_☉ in a distribution similar to that of the CO, but more extended. We compare profiles of CO and H_2 around six molecular peaks; on average H_2 is more extended than CO by a factor of ~1.3. The implied CO-to-H_2 conversion factor ...
Comment: 54 pages in total, 18 figures (21 files) and 4 tables, to appear in
Astrophysical Journal Supplement Series. A full color version with higher
resolution figures is available at
http://www.a.phys.nagoya-u.ac.jp/~kawamura/research/NANTEN_LMC_1_preprint_highres.pdf
We have discovered a molecular dome-like feature towards $355^{\circ} \leq l
\leq 359^{\circ}$ and $0^{\circ} \leq b \leq 2^{\circ}$. The large velocity
dispersions of 50--100 km s$^{-1}$ of this feature are much larger than those
in the Galactic disk and indicate that the feature is located in the Galactic
center, probably within $\sim1$ kpc of Sgr A$^{*}$. The distribution has a
projected length of $\sim600$ pc and height of $\sim300$ pc from the Galactic
disk and shows a large-scale monotonic velocity gradient of $\sim130$ km s
$^{-1}$ per $\sim600$ pc. The feature is also associated with HI gas having a
more continuous spatial and velocity distribution than that of $^{12}$CO. We
interpret the feature as a magnetically floated loop similar to loops 1 and 2
and name it "loop 3". Loop 3 is similar to loops 1 and 2 in its height and
...
Comment: 40 pages, 22 figures, submitted to publication in PASJ
