變色杜定分子雲 I

探索宇宙¹！逐工會揀一幅無仝款 ê 影像抑是相片，𤆬你熟似咱這个迷人 ê 宇宙，閣有專業天文學者²為你解說³。

• 原始文章：Chamaeleon I Molecular Cloud
• 影像來源 kah 版權：Amiel Contuliano
• 台文翻譯：An-Li Tsai (NSYSU)

變色杜定分子雲 I

這幅望遠鏡南天景色內底有 烏-mih-mà ê 烏雲 kah 光-iàⁿ-iàⁿ ê 星雲。 這表示講遮有足濟少年恆星，恆星形成 ê 活動嘛 真鬧熱。 In chhāi tī 干焦 650 光年遠 ê 所在爾爾，踮 變色杜定分子雲複合體 kah 本地波 ê 邊界。 Tī 1946 年編 ê Cederblad 目錄內底，有少年恆星 ê 恆星形成區 去予當做是厚塗粉 ê 反射星雲。 這个目錄內底閣有 C-形 ê Cederblad 110，to̍h tī 相片倒爿中央。 藍色 ê Cederblad 111 to̍h tī 伊 ê 下跤。 這張相片內底閣有一个足顯目 ê 部份，是 柑仔色、V-形 ê 變色杜定紅外線星雲 (Cha IRN)。 彼是去予新形成 ê 低質量恆星 ê 物質流 kā 雕出來 ê 形體。 這幅構圖袂䆀 ê 影像 有 1.5 度闊。 用附近 ê 變色杜定分子雲 I ê 距離來推算，這差不多是 17 光年闊。

[POJ] Piàn-sek-tō͘-tēng hūn-chú-hûn I

Chit-pak bōng-oán-kiàⁿ lâm-thian kéng-sek lāi-té ū o͘-mih-mà ê o͘-hûn kah kng-iàⁿ-iàⁿ ê seng-hûn. Che piáu-sī kóng chiah ū chiok-chōe siàu-liân hêng-chhiⁿ, hêng-chhiⁿ hêng-sêng ê oa̍h-tāng mā chin nāu-jia̍t. In chhāi tī kan-na 650 kng-nî hn̄g ê só͘-chāi niā-niā, tiàm Piàn-sek-tō͘-tēng hūn-chú-hûn ho̍k-ha̍p-thé kah Pún-tē-pho ê pian-kài. Tī 1946 nî pian ê Cederblad bo̍k-lo̍k lāi-té, ū siàu-liân hêng-chhiⁿ ê hêng-chhiⁿ hêng-sêng-khu khì hō͘ tòng-chòe sī kāu-thô͘-hún ê hoán-siā-seng-hûn. Chi̍t-ê bo̍k-lo̍k lāi-té koh ū C-hêng ê Ced 110, to̍h tī siòng-phìⁿ tò-pêng tiong-ng. Nâ-sek ê Ced 111 to̍h tī i ê ē-kha. Chit-tiuⁿ siòng-phìⁿ lāi-té koh ū chi̍t-ê chiok hiáⁿ-ba̍k ê pō͘-hūn, sī kam-á-sek, V-hêng ê Piàn-sek-tō͘-tēng Âng-gōa-sòaⁿ seng-hûn (Cha IRN). He sī khì hō͘ sin hêng-sêng ê kē-chit-liōng hêng-chhiⁿ ê bu̍t-chit-liû kā tiau--chhut-lâi ê hêng-thé. Chit-pak kó͘-tô͘ bōe-bái ê iáⁿ-siōng ū 1.5 tō͘ khoah. Iōng hū-kīn ê Piàn-sek-tō͘-tēng hūn-chú-hûn I ê kū-lî lâi thui-sǹg, che chha-put-to sī 17 kng-nî khoah.

[KIP] Piàn-sik-tōo-tīng hūn-tsú-hûn I

Tsit-pak bōng-uán-kiànn lâm-thian kíng-sik lāi-té ū oo-mih-mà ê oo-hûn kah kng-iànn-iànn ê sing-hûn. Tse piáu-sī kóng tsiah ū tsiok-tsuē siàu-liân hîng-tshinn, hîng-tshinn hîng-sîng ê ua̍h-tāng mā tsin nāu-jia̍t. In tshāi tī kan-na 650 kng-nî hn̄g ê sóo-tsāi niā-niā, tiàm Piàn-sik-tōo-tīng hūn-tsú-hûn ho̍k-ha̍p-thé kah Pún-tē-pho ê pian-kài. Tī 1946 nî pian ê Cederblad bo̍k-lo̍k lāi-té, ū siàu-liân hîng-tshinn ê hîng-tshinn hîng-sîng-khu khì hōo tòng-tsuè sī kāu-thôo-hún ê huán-siā-sing-hûn. Tsi̍t-ê bo̍k-lo̍k lāi-té koh ū C-hîng ê Ced 110, to̍h tī siòng-phìnn tò-pîng tiong-ng. Nâ-sik ê Ced 111 to̍h tī i ê ē-kha. Tsit-tiunn siòng-phìnn lāi-té koh ū tsi̍t-ê tsiok hiánn-ba̍k ê pōo-hūn, sī kam-á-sik, V-hîng ê Piàn-sik-tōo-tīng Âng-guā-suànn sing-hûn (Tsa IRN). He sī khì hōo sin hîng-sîng ê kē-tsit-liōng hîng-tshinn ê bu̍t-tsit-liû kā tiau--tshut-lâi ê hîng-thé. Tsit-pak kóo-tôo buē-bái ê iánn-siōng ū 1.5 tōo khuah. Iōng hū-kīn ê Piàn-sik-tōo-tīng hūn-tsú-hûn I ê kū-lî lâi thui-sǹg, tse tsha-put-to sī 17 kng-nî khuah.

[English] Chamaeleon I Molecular Cloud

Dark markings and bright nebulae in this telescopic southern sky view are telltale signs of young stars and active star formation. They lie a mere 650 light-years away, at the boundary of the local bubble and the Chamaeleon molecular cloud complex. Regions with young stars identified as dusty reflection nebulae from the 1946 Cederblad catalog include the C-shaped Ced 110 just above and right of center, and bluish Ced 111 below it. Also a standout in the frame, the orange tinted V-shape of the Chamaeleon Infrared Nebula (Cha IRN) was carved by material streaming from a newly formed low-mass star. The well-composed image spans 1.5 degrees. That's about 17 light-years at the estimated distance of the nearby Chamaeleon I molecular cloud.

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