论文标题
高质量，多阶段形成区域IRA的红外研究IRA 〜12272-6240
An infrared study of the high-mass, multi-stage star-forming region IRAS~12272-6240
论文作者
论文摘要
IRAS 12272-6240是一个复杂的恒星形成区域，具有紧凑的大块浓密团块，几个相关的masers，位于$ d = 9.3 $ kpc的确定距离。在这项研究中，我们通过Baade/Magellan望远镜及其相机恐慌获得了亚弧形宽带和狭窄的近红外成像和低分辨率光谱。 $ 2 \ times 2 $ Square Arcmin的马赛克在$ JHK_S $频段中以及以2.12 $ $ $ m h $ _2 $和2.17 $ $ m $ m $ $ u量的滤波器为中心，与hi-gal/{\ sl herschel}和Spits and spit和Spit}和Spit}和Spit}一起分析观察。我们发现，紧凑型浓密的团块容纳了可能形成21 KAU范围二进制系统的两个类别。它的合并1至1200 $μ$ m sed与$ 10^{ - 2} m_ \ odot $ disc和$ 1.3 \ times 10^4 m_ \ odot $ dust $ duck unvelope一致的O9V中心星一致。它的总亮度为$ 8.5 \ times 10^4 l_ \ odot $。在附近发现了一系列震惊的H $ _2 $发射结，证实了流出的存在。 IRAS 12272-6240位于嵌入式簇的中心，平均年龄为1 MYR，大小为2.6 PC，其中包含超过150颗恒星。在其核上，我们发现一个含有YSO的更年轻，更年轻的亚簇。我们还鉴定并分类了两个尘土飞播/IR HII区域的O型中心星，该恒星侧面是质恒定的。我们的结果证实，这些元素形成了一个巨大的年轻综合体，大约在100万年前开始了大规模的恒星形成过程，并且仍然活跃。
IRAS 12272-6240 is a complex star forming region with a compact massive dense clump and several associated masers, located at a well-determined distance of $d=9.3$ kpc from the Sun. For this study, we obtained sub-arcsec broad- and narrow-band near-IR imaging and low-resolution spectroscopy with the Baade/Magellan telescope and its camera PANIC. Mosaics of size $2 \times 2$ square arcmin in the $JHK_s$ bands and with narrow-band filters centred in the 2.12 $μ$m H$_2$ and 2.17 $μ$m Br$γ$ lines were analysed in combination with HI-GAL/{\sl Herschel} and archive IRAC/{\sl Spitzer} and {\sl WISE} observations. We found that the compact dense clump houses two Class~I YSOs that probably form a 21 kAU-wide binary system. Its combined 1 to 1200 $μ$m SED is consistent with an O9V central star with a $10^{-2} M_\odot$ disc and a $1.3 \times 10^4 M_\odot$ dust envelope. Its total luminosity is $8.5 \times 10^4 L_\odot$. A series of shocked H$_2$ emission knots are found in its close vicinity, confirming the presence of outflows. IRAS 12272-6240 is at the centre of an embedded cluster with a mean age of 1 Myr and 2.6 pc in size that contains more than 150 stars. At its nucleus, we found a more compact and considerably younger sub-cluster containing the YSOs. We also identified and classified the O-type central stars of two dusty radio/IR HII regions flanking the protostars. Our results confirm that these elements form a single giant young complex where massive star formation processes started some 1 million years ago and is still active.
