NGC 1705 a | Haro 11 a | Mrk 1089 | ||
![]() ![]() ![]() |
(1) | 5.8 ![]() |
1.7 ![]() |
3.9 ![]() |
(2) | 4.9 ![]() |
1.4 ![]() |
3.8 ![]() |
|
(3) | 5.9 ![]() |
1.6 ![]() |
4.3 ![]() |
|
![]() ![]() |
1.9 ![]() |
1.2 ![]() |
1.4 ![]() |
|
![]() ![]() |
2.2 ![]() |
4.1 ![]() |
1.3 ![]() |
|
![]() ![]() |
1.6 ![]() |
9.6 ![]() |
1.1 ![]() |
|
![]() ![]() ![]() |
5.1 ![]() |
1.6 ![]() |
3.7 ![]() |
|
![]() |
6.34 ![]() |
3.2 ![]() |
4.57 ![]() |
|
Size | 0.5' ![]() |
0.25' ![]() |
0.31' ![]() |
|
SFR (![]() |
(4) | 1.6 ![]() |
5.1 ![]() |
5 ![]() |
(5) | 9.4 ![]() |
- | 5.8 ![]() |
|
(6) | 5.2 ![]() |
2.4 ![]() |
1.4 ![]() |
|
(7) | 5.7 ![]() |
3 ![]() |
1.8 ![]() |
a The models used for
NGC 1705 and Haro 11 include an independent, very
cold dust component at 10 K with an emissivity = 1.
b Total infrared luminosities
(
)
are estimated: 1) by integrating our SED models with a submm
constraint from 3 to 1100
m; 2) from the Dale & Helou (2002)
formula; 3) from the Draine
& Li (2007) formula.
c H
luminosities (
)
are given in Cannon
et al. (2006) for NGC 1705, Bergvall et al. (2000)
for Haro 11 and c) Iglesias-Paramo
& Vilchez (1997) for Mrk 1089.
d Star formation rates (SFR)
are estimated: 4) using the relation of Kennicutt (1998) based on
;
5) using the relation of Zhu
et al. (2008) based on
[24
m]. (this
last relation is only valid for galaxies with a
<
10
and can not be used for
Haro 11); 6) using the
relation of Calzetti (2007)
based on the 24
m
luminosity (L24)
alone; 7) using the relation of Calzetti
(2007) based on L24
and
.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.