仙王座內底 ê NGC 7822 星雲

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：NGC 7822 in Cepheus
• 影像來源 kah 版權：Mark Carter
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] 仙王座內底 ê NGC 7822 星雲

NGC 7822 星雲內底應該是有足濟高溫少年 ê 恆星 kah 氣體塗粉做 ê 宇宙柱仔雲。 伊 to̍h tī 北天星座仙王座內底 ê 巨型分子雲邊仔，是一个離咱差不多 3000 光年遠、leh 發光 ê 恆星形成區。 這个星雲有較光 ê 邊界 kah 烏暗 ê 外形。 Tùi 這幅用 望遠鏡翕 ê 彩色天景 來講，實在是足出眾 ê。 這張影像內底有 狹頻 濾鏡 ê 觀測資料，kā 酸素原子、水素原子、kah 硫磺原子 ê 發射線，用做藍色、青色、kah 紅色色調。 發射線 kah 色光 ê 組合就是咱熟似 ê 哈伯色盤。 原子發射線 是去予恆星形成區中央 ê 高溫恆星 ê 高能輻射 kā 激發出來 ê 。 足強 ê 恆星風 kah 輻射，毋若 kā 實密 ê 柱仔雲形體 雕出來，閣 kā 修修 leh。 而且閣 tī 這个製造恆星 ê 星雲區中央，掃出一个 幾若光年闊 ê 特殊 閬空。 這个柱仔雲會因為 重力崩塌，繼續做新 ê 恆星出來。 毋閣等到柱仔雲去予侵蝕了了，to̍h 無法度 tī 這个 恆星原料場 閣製造新 ê 恆星矣。 用 NGC 7822 ê 距離來估算，這个視野差不多有 40 光年闊。

[POJ] Sian-ông-chō lāi-té ê NGC chhit-pat-jī-jī seng-hûn

NGC chhit-pat-jī-jī seng-hûn lāi-té eng-kai sī ū chiok-chōe ko-un siàu-liân ê hêng-chhiⁿ kah khì-thé thô͘-hún chò ê ú-tiū thiāu-á-hûn. I to̍h tī pak-thian seng-chō Sian-ông-chō lāi-té ê kū-hêng hūn-chú-hûn piⁿ-á, sī chi̍t-ê lî lán chha-put-to saⁿ-chheng kng-nî hn̄g, leh hoat-kng ê hêng-chhiⁿ hêng-sêng-khu. Chit-ê seng-hûn ū khah kng ê pian-kài kah o͘-àm ê gōa-hêng. Tùi chit-pak iōng bōng-oán-kiàⁿ hip ê chhái-sek thian-kéng lâi-kóng, si̍t-chāi sī chiok chhut-chiòng ê. Chit-tiuⁿ iáⁿ-siōng lāi-té ū e̍h-pîn lū-kiàⁿ ê koan-chhek chu-liāu, kā sng-sò͘ goân-chú, chúi-sò͘ goân-chú, kah liû-hông goân-chú ê hoat-siā-sòaⁿ, iōng chò nâ-sek, chhiⁿ-sek, kah âng-sek sek-tiāu. Hoat-siā-sòaⁿ kah se̍k-kng ê cho͘-ha̍p tō-sī lán se̍k-sāi ê Ha-peh sek-pôaⁿ. Goân-chú hoat-siā-sòaⁿ sī khì hō͘ hêng-chhiⁿ hêng-sêng-khu tiong-ng ê ko-un hêng-chhiⁿ ê ko-lêng hok-siā kā kek-hoat chhut-lâi ê. Chiok kiông ê hêng-chhiⁿ-hong kah hok-siā, m̄-nā kā cha̍t-ba̍t ê thiāu-á-hûn hêng-thé tiau--chut-lâi, koh kā siu-siu-leh. Jî-chhiáⁿ koh tī chit-ê chè-chō hêng-chhiⁿ ê seng-hûn-khu tiong-ng, sàu chhut chi̍t-ê kúi-ā kng-nî khoah ê te̍k-siá làng-khong. Chit-ê thiāu-á-hûn ē in-ūi tiōng-le̍k pang-lap, kè-sio̍k chò sin ê hêng-chhiⁿ chhut-lâi. M̄-koh tán kàu thiāu-á-hûn khì hō͘ chhim-sit liáu-liáu, to̍h bô-hoat-tō͘ tī chit-ê hêng-chhiⁿ goân-liāu-tiûⁿ koh chè-chō sin ê hêng-chhiⁿ ah. Iōng NGC chhit-pat-jī-jī ê kū-lî lâi kó͘-sǹg, chit-ê sī-iá chha-put-to ū sì-cha̍p kng-nî khoah.

[KIP] Sian-ông-tsō lāi-té ê NGC tshit-pat-jī-jī sing-hûn

NGC tshit-pat-jī-jī sing-hûn lāi-té ing-kai sī ū tsiok-tsuē ko-un siàu-liân ê hîng-tshinn kah khì-thé thôo-hún tsò ê ú-tiū thiāu-á-hûn. I to̍h tī pak-thian sing-tsō Sian-ông-tsō lāi-té ê kū-hîng hūn-tsú-hûn pinn-á, sī tsi̍t-ê lî lán tsha-put-to sann-tshing kng-nî hn̄g, leh huat-kng ê hîng-tshinn hîng-sîng-khu. Tsit-ê sing-hûn ū khah kng ê pian-kài kah oo-àm ê guā-hîng. Tuì tsit-pak iōng bōng-uán-kiànn hip ê tshái-sik thian-kíng lâi-kóng, si̍t-tsāi sī tsiok tshut-tsiòng ê. Tsit-tiunn iánn-siōng lāi-té ū e̍h-pîn lū-kiànn ê kuan-tshik tsu-liāu, kā sng-sòo guân-tsú, tsuí-sòo guân-tsú, kah liû-hông guân-tsú ê huat-siā-suànn, iōng tsò nâ-sik, tshinn-sik, kah âng-sik sik-tiāu. Huat-siā-suànn kah si̍k-kng ê tsoo-ha̍p tō-sī lán si̍k-sāi ê Ha-peh sik-puânn. Guân-tsú huat-siā-suànn sī khì hōo hîng-tshinn hîng-sîng-khu tiong-ng ê ko-un hîng-tshinn ê ko-lîng hok-siā kā kik-huat tshut-lâi ê. Tsiok kiông ê hîng-tshinn-hong kah hok-siā, m̄-nā kā tsa̍t-ba̍t ê thiāu-á-hûn hîng-thé tiau--tsut-lâi, koh kā siu-siu-leh. Jî-tshiánn koh tī tsit-ê tsè-tsō hîng-tshinn ê sing-hûn-khu tiong-ng, sàu tshut tsi̍t-ê kuí-ā kng-nî khuah ê ti̍k-siá làng-khong. Tsit-ê thiāu-á-hûn ē in-uī tiōng-li̍k pang-lap, kè-sio̍k tsò sin ê hîng-tshinn tshut-lâi. M̄-koh tán kàu thiāu-á-hûn khì hōo tshim-sit liáu-liáu, to̍h bô-huat-tōo tī tsit-ê hîng-tshinn guân-liāu-tiûnn koh tsè-tsō sin ê hîng-tshinn ah. Iōng NGC tshit-pat-jī-jī ê kū-lî lâi kóo-sǹg, tsit-ê sī-iá tsha-put-to ū sì-tsa̍p kng-nî khuah.

[English] NGC 7822 in Cepheus

Hot, young stars and cosmic pillars of gas and dust seem to crowd into NGC 7822. At the edge of a giant molecular cloud toward the northern constellation Cepheus, the glowing star forming region lies about 3,000 light-years away. Within the nebula, bright edges and dark shapes stand out in this colorful telescopic skyscape. The image includes data from narrowband filters, mapping emission from atomic oxygen, hydrogen, and sulfur into blue, green, and red hues. The emission line and color combination has become well-known as the Hubble palette. The atomic emission is powered by energetic radiation from the central hot stars. Their powerful winds and radiation sculpt and erode the denser pillar shapes and clear out a characteristic cavity light-years across the center of the natal cloud. Stars could still be forming inside the pillars by gravitational collapse but as the pillars are eroded away, any forming stars will ultimately be cutoff from their reservoir of star stuff. This field of view spans about 40 light-years at the estimated distance of NGC 7822.

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