少年星團 NGC 346

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• 原始文章：Young Star Cluster NGC 346
• 影像來源：科學：NASA, ESA, CSA, Olivia C. Jones (UK ATC), Guido De Marchi (ESTEC), Margaret Meixner (USRA)； 資料： Alyssa Pagan (STScI), Nolan Habel (USRA), Laura Lenkić (USRA), Laurie E. U. Chu (NASA Ames)
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] 少年星團 NGC 346

質量上大 ê 少年星團是 NGC 346。 伊就 tī 咱 ê 衛星星系 小麥哲倫星雲 ê 恆星形成區內底，離咱有 21 萬光年遠。 雖罔講 NGC 346 星團內底 ê 大質量恆星 攏足短命--ê，毋過 in 攏 活跳跳 閣 pìn-piàng 叫。 恆星風 kah 輻射 leh 雕這區 厚塗粉 分子雲外沿 ê 時陣，會驅動內底 ê 恆星形成活動。 恆星形成區內底會有足濟 紅嬰仔恆星，四散 tī 星團內底。 In 才 300 到 500 萬歲爾爾，猶未開始 tī in ê 核心 進行 水素 ê 核融合反應。 NGC 346 這張壯觀 ê 紅外線景色 是 ùi James Webb 太空望遠鏡 ê 近紅外線相機 NIRcam 翕--ê。 相片內底 ê 粉紅仔色，是大質量恆星 ê 高能輻射 kā 水素原子 離子化。 柑仔色是恆星形成分子雲 內底 ê 水素分子 kah 塗粉 發出 ê 發射線。 Webb 太空望遠鏡翕--ê 這張 遮爾清楚 ê 少年恆星形成區，若是照 小麥哲倫星雲 ê 距離來估算，應該是有 240 光年闊。

[POJ] Siàu-liân Seng-thoân NGC 346

Chit-liōng siōng tōa ê siàu-liân seng-thoân sī NGC 346. I to̍h tī lán ê ōe-chheⁿ seng-hē Sió Be̍h-tiat-lûn Seng-hûn ê hêng-chheⁿ hêng-sêng-khu lāi-té, lī lán ū 21 bān kng-nî hn̄g. Sui-bóng kóng NGC 346 seng-thoân lāi-té ê tōa-chit-liōng hêng-chheⁿ lóng chiok té-miā--ê, m̄-koh in lóng oa̍h-thiàu-thiàu koh pìn-piàng kiò. Hêng-chheⁿ-hong kah hok-siā leh tiau chit-khu kāu thô͘-hún hun-chú-hûn gōa-iân ê sî-chūn, ē khu-tōng lāi-té ê hêng-chheⁿ hêng-sêng oa̍h-tōng. Hêng-chheⁿ hêng-sêng-khu lāi-té ē ū chiok chōe âng-eⁿ-á hêng-chheⁿ, sì-sòaⁿ tī seng-thoân lāi-té. In chiah 300 kàu 500 bān hòe niā-niā, iáu-bē khai-sí tī in ê he̍k-sim chìn-hêng chúi-sò͘ ê he̍k-iông-ha̍p hoán-èng. NGC 346 chit tiuⁿ chòng-koan ê âng-gōa-sòaⁿ kéng-sek sī ùi James Webb Thài-khong Bōng-oán-kiàⁿ ê kīn-âng-gōa-sòaⁿ siòng-ki NIRcam hip--ê. Siòng-phìⁿ lāi-té ê hún-âng-á-sek, sī tōa-chit-liōng hêng-chheⁿ ê ko-lêng hok-siā kā chúi-sò͘ goân-chú lī-chú-hòa. Kam-á-sek sī hêng-chheⁿ hêng-sêng hun-chú-hûn lāi-té ê chúi-sò͘ hun-chú kah thô͘-hún hoat--chhut ê hoat-siā-sòaⁿ. Webb Thài-khong Bōng-oán-kiàⁿ hip--ê chit-tiuⁿ chiah-nī chheng-chhó ê siàu-liân hêng-chheⁿ hêng-sêng-khu, nā-sī chiàu Sió Be̍h-tiat-lûn Seng-hûn ê kū-lī lâi kó͘-sǹg, èng-kai sī ū 240 kng-nî khoah.

[KIP] Siàu-liân Sing-thuân NGC 346

Tsit-liōng siōng tuā ê siàu-liân sing-thuân sī NGC 346. I to̍h tī lán ê uē-tshenn sing-hē Sió Be̍h-tiat-lûn Sing-hûn ê hîng-tshenn hîng-sîng-khu lāi-té, lī lán ū 21 bān kng-nî hn̄g. Sui-bóng kóng NGC 346 sing-thuân lāi-té ê tuā-tsit-liōng hîng-tshenn lóng tsiok té-miā--ê, m̄-koh in lóng ua̍h-thiàu-thiàu koh pìn-piàng kiò. Hîng-tshenn-hong kah hok-siā leh tiau tsit-khu kāu thôo-hún hun-tsú-hûn guā-iân ê sî-tsūn, ē khu-tōng lāi-té ê hîng-tshenn hîng-sîng ua̍h-tōng. Hîng-tshenn hîng-sîng-khu lāi-té ē ū tsiok tsuē âng-enn-á hîng-tshenn, sì-suànn tī sing-thuân lāi-té. In tsiah 300 kàu 500 bān huè niā-niā, iáu-bē khai-sí tī in ê hi̍k-sim tsìn-hîng tsuí-sòo ê hi̍k-iông-ha̍p huán-ìng. NGC 346 tsit tiunn tsòng-kuan ê âng-guā-suànn kíng-sik sī uì James Webb Thài-khong Bōng-uán-kiànn ê kīn-âng-guā-suànn siòng-ki NIRcam hip--ê. Siòng-phìnn lāi-té ê hún-âng-á-sik, sī tuā-tsit-liōng hîng-tshenn ê ko-lîng hok-siā kā tsuí-sòo guân-tsú lī-tsú-huà. Kam-á-sik sī hîng-tshenn hîng-sîng hun-tsú-hûn lāi-té ê tsuí-sòo hun-tsú kah thôo-hún huat--tshut ê huat-siā-suànn. Webb Thài-khong Bōng-uán-kiànn hip--ê tsit-tiunn tsiah-nī tshing-tshó ê siàu-liân hîng-tshenn hîng-sîng-khu, nā-sī tsiàu Sió Be̍h-tiat-lûn Sing-hûn ê kū-lī lâi kóo-sǹg, ìng-kai sī ū 240 kng-nî khuah.

[English] Young Star Cluster NGC 346

The most massive young star cluster in the Small Magellanic Cloud is NGC 346, embedded in our small satellite galaxy's largest star forming region some 210,000 light-years distant. Of course the massive stars of NGC 346 are short lived, but very energetic. Their winds and radiation sculpt the edges of the region's dusty molecular cloud triggering star-formation within. The star forming region also appears to contain a large population of infant stars. A mere 3 to 5 million years old and not yet burning hydrogen in their cores, the infant stars are strewn about the embedded star cluster. This spectacular infrared view of NGC 346 is from the James Webb Space Telescope's NIRcam. Emission from atomic hydrogen ionized by the massive stars' energetic radiation as well as and molecular hydrogen and dust in the star-forming molecular cloud is detailed in pink and orange hues. Webb's sharp image of the young star-forming region spans 240 light-years at the distance of the Small Magellanic Cloud.

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