M102：坦倒 ê 側向盤仔型星系

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：M102: Edge-on Disk Galaxy
• 影像來源：NASA, ESA, Hubble; 資料處理：Ehsan Ebrahimian
• 台文翻譯：An-Li Tsai (NSYSU)

[漢羅] M102：坦倒 ê 側向盤仔型星系

這是啥物天體？ 這是一个正常星系，毋過是坦倒 ê 側向星系。 足濟盤仔型星系實際上 kah 相片 內底 ê NGC 5866 紡錘星系 平薄，毋過 ùi 咱 ê 方向來看，in 毋是坦倒--ê。 其實咱閣較熟似 ê 側向星系，應該是咱 ê 銀河系。 紡錘星系 ê 另外一个編號是 M102，伊有足濟足複雜 ê 塗粉帶，tī 相片內底是較暗較烏 ê 部份。 星系盤內底較光 ê 恆星，予星系看起來變做是藍色--ê。 咱會當 tī 哈伯 影像內底 看著有少年 恆星 ê 藍色星系盤，伊延伸 ê 範圍比這个 足薄 ê 星系盤 ê 塗粉 閣較闊。 有證據講這个 紡錘 星系 tī 過去幾若十億年 ê 時間內，捌 kā 幾若个較細 ê 星系食食去。 包括 幾若條較暗 ê 恆星流，離星系盤較遠 ê 烏暗塗粉，kah 踅 tī 週邊、毋過無出現 tī 相片內底 ê 星系群。 一般講來，足濟 盤仔型星系會變薄，因為 形成盤仔 ê 氣體 tī 踅重力中心 ê 時陣會相挵。 紡錘星系 就 tī 天龍座 方向 5000 萬 光年 遠 ê 所在。

[POJ] M102: Thán-tó ê chhek-hiòng pôaⁿ-á hêng seng-hē

Che-sī siáⁿ-mih thian-thé? Che-sī chi̍t-ê chèng-siông seng-hē, m̄-koh sī thán-tó ê chhek-hiòng seng-hē. Chiok chē pôaⁿ-á-hêng seng-hē si̍t-chè-siōng kah siòng-phìⁿ lāi-té ê NGC 5866 Pháng-thûi Seng-hē pêⁿ po̍h, m̄-koh ùi lán ê hong-hiòng lâi-khòaⁿ, in m̄-sī thán-tó--ê. Kî-si̍t lán koh-khah se̍k-sāi ê chhek-hiòng seng-hē, eng-kai sī lán ê Gîn-hô-hē. Pháng-thûi Seng-hē ê lēng-gōa chi̍t-ê pian-hō sī M102, i ū chiok chē chiok ho̍k-cha̍p ê thô͘-hún-tòa, tī siòng-phìⁿ lāi-té sī khah àm khah o͘ ê pō͘-hūn. Seng-hē-pôaⁿ lāi-té khah kng ê hêng-chheⁿ, hō͘ seng-hē khòaⁿ--khí-lâi piàn-chò sī nâ-sek--ê. Lán ē-tàng tī Ha-peh iáⁿ-siōng lāi-té khòaⁿ-tio̍h ū siàu-liân hêng-chheⁿ ê nâ-sek seng-hē-pôaⁿ, i iân-sin ê hoān-ûi pí chit-ê chiok po̍h ê seng-hē-pôaⁿ ê thô͘-hún koh-khah khoah. Ū chèng-kì kóng chit-ê Pháng-thûi Seng-hē tī kòe-khì kúi-nā cha̍p-ek nî ê sî-kan-lāi, bat kā kúi-nā ê khah sè ê seng-hē chia̍h-chia̍h-khì. Pau-koat kúi-nā tiâu khah àm ê hêng-chheⁿ-liû, lī seng-hē-pôaⁿ khah hn̄g ê o͘-àm thô͘-hún, kah se̍h tī chiu-piⁿ, m̄-koh bô chhut-hiān tī siòng-phìⁿ lāi-té ê seng-hē-kûn. It-poaⁿ kóng-lâi, chiok chē pôaⁿ-á-hêng seng-hē ē piàn po̍h, in-ūi hêng-sêng pôaⁿ-á ê khì-thé tī se̍h tiong-le̍k tiong-sim ê sî-chūn ē sio-lòng. Pháng-thûi Seng-hē to̍h tī Thian-liông-chō hong-hiòng 5000 bān kng-nî hn̄g ê só͘-chāi.

[KIP] M102: Thán-tó ê tshik-hiòng puânn-á hîng sing-hē

Tse-sī siánn-mih thian-thé? Tse-sī tsi̍t-ê tsìng-siông sing-hē, m̄-koh sī thán-tó ê tshik-hiòng sing-hē. Tsiok tsē puânn-á-hîng sing-hē si̍t-tsè-siōng kah siòng-phìnn lāi-té ê NGC 5866 Pháng-thuî Sing-hē pênn po̍h, m̄-koh uì lán ê hong-hiòng lâi-khuànn, in m̄-sī thán-tó--ê. Kî-si̍t lán koh-khah si̍k-sāi ê tshik-hiòng sing-hē, ing-kai sī lán ê Gîn-hô-hē. Pháng-thuî Sing-hē ê līng-guā tsi̍t-ê pian-hō sī M102, i ū tsiok tsē tsiok ho̍k-tsa̍p ê thôo-hún-tuà, tī siòng-phìnn lāi-té sī khah àm khah oo ê pōo-hūn. Sing-hē-puânn lāi-té khah kng ê hîng-tshenn, hōo sing-hē khuànn--khí-lâi piàn-tsò sī nâ-sik--ê. Lán ē-tàng tī Ha-peh iánn-siōng lāi-té khuànn-tio̍h ū siàu-liân hîng-tshenn ê nâ-sik sing-hē-puânn, i iân-sin ê huān-uî pí tsit-ê tsiok po̍h ê sing-hē-puânn ê thôo-hún koh-khah khuah. Ū tsìng-kì kóng tsit-ê Pháng-thuî Sing-hē tī kuè-khì kuí-nā tsa̍p-ik nî ê sî-kan-lāi, bat kā kuí-nā ê khah sè ê sing-hē tsia̍h-tsia̍h-khì. Pau-kuat kuí-nā tiâu khah àm ê hîng-tshenn-liû, lī sing-hē-puânn khah hn̄g ê oo-àm thôo-hún, kah se̍h tī tsiu-pinn, m̄-koh bô tshut-hiān tī siòng-phìnn lāi-té ê sing-hē-kûn. It-puann kóng-lâi, tsiok tsē puânn-á-hîng sing-hē ē piàn po̍h, in-uī hîng-sîng puânn-á ê khì-thé tī se̍h tiong-li̍k tiong-sim ê sî-tsūn ē sio-lòng. Pháng-thuî Sing-hē to̍h tī Thian-liông-tsō hong-hiòng 5000 bān kng-nî hn̄g ê sóo-tsāi.

[English] M102: Edge-on Disk Galaxy

What kind of celestial object is this? A relatively normal galaxy -- but seen from its edge. Many disk galaxies are actually just as thin as NGC 5866, the Spindle galaxy, pictured here, but are not seen edge-on from our vantage point. A perhaps more familiar galaxy seen edge-on is our own Milky Way galaxy. Also cataloged as M102, the Spindle galaxy has numerous and complex dust lanes appearing dark and red, while many of the bright stars in the disk give it a more blue underlying hue. The blue disk of young stars can be seen in this Hubble image extending past the dust in the extremely thin galactic plane. There is evidence that the Spindle galaxy has cannibalized smaller galaxies over the past billion years or so, including multiple streams of faint stars, dark dust that extends away from the main galactic plane, and a surrounding group of galaxies (not shown). In general, many disk galaxies become thin because the gas that forms them collides with itself as it rotates about the gravitational center. The Spindle galaxy lies about 50 million light years distant toward the constellation of the Dragon (Draco).

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