熔做愛因斯坦環 ê 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：A Molten Galaxy Einstein Ring
• 影像來源：ESA/Hubble & NASA, S. Jha; 資料處理：Jonathan Lodge
• 阿拉伯語 ê APOD：面冊, Instagram, kah Twitter
• 台文翻譯：An-Li Tsai (NCU)

[漢羅] 熔做愛因斯坦環 ê 星系

欲 kā 星系藏踮星系團後壁實在是無可能 ê 代誌。 附近若是有一个星系團，伊 ê 引力就親像是一个 巨型 ê 透鏡，會 kā 彼附近仝款 遙遠 ê 星系 影像 搝甲完全變形。 這張相片 就是按呢。 這是最近才 kā Hubble 太空望遠鏡 觀測過 ê 影像 重新處理過--ê。 這个星系團叫做 GAL-CLUS-022058c，內底有幾若个星系，利用 重力透鏡效應 kā 背景星系 ê 影像拗彎做影像中央柑仔色 ê 光弧。 因為 伊 ê 形體遮爾奇怪，去 hŏng 叫做是 熔去的 愛因斯坦環，內底會當揣著四个 ùi 仝一个背景星系來 ê 影像。 一般講來，前景星系團內底大部份 ê 質量 分佈愛平均，才有法度產生遮爾滑溜 ê 光弧。 所以星系團 ê 質量分佈，應該毋是干焦你目睭看著 ê 部份爾爾。 分析這寡 重力弧 ê 位置，會當提供天文學家估計星系團內底 烏暗物質 分佈 ê 情形，嘛會當推測恆星 tī 這寡早期星系內底是按怎開始形成--ê。

[POJ] Iûⁿ chò Ài-in-su-thán-khoân ê seng-hē

Beh kā seng-hē chhàng tiàm seng-hē-thoân āu-piah si̍t-chāi sī bô-khó-lêng ê tāi-chì. Hù-kīn nā-sī ū chi̍t-ê seng-hē-thoân, i ê ín-le̍k to̍h chhin-chhiūⁿ sī chi̍t-ê kū-hêng ê thàu-kiàⁿ, ē kā hū-kīn kāng-khoán iâu-oán ê seng-hē iáⁿ-siōng giú kah oân-choân piàn-hêng. Chit tiuⁿ siòng-phìⁿ to̍h sī án-ne. Che sī chòe-kīn chiah kā Hubble Thài-khong-bōng-oán-kiàⁿ koan-chhek kòe ê iáⁿ-siōng tiông-sin chhú-lí kòe--ê. Chit ê seng-hē-thoân kiò-chò GAL-CLUS-022058c, lāi-té ū kúi-ā-ê seng-hē, lī-iōng tiōng-le̍k-thàu-kiàⁿ hāu-èng kā pōe-kéng seng-hē ê iáⁿ-siōng áu-oan chò iáⁿ-siōng tiong-ng kam-á-sek ê kng-hô͘. In-ūi i ê hêng-thé chiah-nī kî-koài, khì hŏng kiò-chò sī iûⁿ--khì ê Ài-in-su-thán-khoân, lāi-té ē-tàng chhōe-tio̍h sì ê ùi kāng chi̍t-ê pōe-kéng seng-hē lâi ê iáⁿ-siōng. It-poaⁿ kóng-lâi, chiân-kéng seng-hē-thoân lāi-té tōa-pō͘-hūn ê chit-liōng hun-pò͘ ài pêng-kun, chiah ū-hoat-tō͘ sán-seng chiah-nī ku̍t-liu ê kng-hô͘. Só͘-í seng-hē-thoân ê chit-liōng hun-pò͘, èng-kai m̄-sī kan-na lí ba̍k-chiu khòaⁿ-tio̍h ê pō͘-hūn niā-niā. Hun-sek chit-kóa tiōng-le̍k-hô͘ ê ūi-tì, ē-tàng thê-kiong thian-bûn ha̍k-ka kó͘-kè seng-hē-thoân lāi-té o͘-àm-bu̍t-chit hun-pò͘ ê chêng-hêng, mā ē-tàng thui-chhek hêng-chhiⁿ tī chit-kóa chá-kî seng-hē lāi-té sī án-ná khai-sí hêng-sêng--ê.

[KIP] Iûnn tsò Ài-in-su-thán-khuân ê sing-hē

Beh kā sing-hē tshàng tiàm sing-hē-thuân āu-piah si̍t-tsāi sī bô-khó-lîng ê tāi-tsì. Hù-kīn nā-sī ū tsi̍t-ê sing-hē-thuân, i ê ín-li̍k to̍h tshin-tshiūnn sī tsi̍t-ê kū-hîng ê thàu-kiànn, ē kā hū-kīn kāng-khuán iâu-uán ê sing-hē iánn-siōng giú kah uân-tsuân piàn-hîng. Tsit tiunn siòng-phìnn to̍h sī án-ne. Tse sī tsuè-kīn tsiah kā Hubble Thài-khong-bōng-uán-kiànn kuan-tshik kuè ê iánn-siōng tiông-sin tshú-lí kuè--ê. Tsit ê sing-hē-thuân kiò-tsò GAL-CLUS-022058c, lāi-té ū kuí-ā-ê sing-hē, lī-iōng tiōng-li̍k-thàu-kiànn hāu-ìng kā puē-kíng sing-hē ê iánn-siōng áu-uan tsò iánn-siōng tiong-ng kam-á-sik ê kng-hôo. In-uī i ê hîng-thé tsiah-nī kî-kuài, khì hŏng kiò-tsò sī iûnn--khì ê Ài-in-su-thán-khuân, lāi-té ē-tàng tshuē-tio̍h sì ê uì kāng tsi̍t-ê puē-kíng sing-hē lâi ê iánn-siōng. It-puann kóng-lâi, tsiân-kíng sing-hē-thuân lāi-té tuā-pōo-hūn ê tsit-liōng hun-pòo ài pîng-kun, tsiah ū-huat-tōo sán-sing tsiah-nī ku̍t-liu ê kng-hôo. Sóo-í sing-hē-thuân ê tsit-liōng hun-pòo, ìng-kai m̄-sī kan-na lí ba̍k-tsiu khuànn-tio̍h ê pōo-hūn niā-niā. Hun-sik tsit-kuá tiōng-li̍k-hôo ê uī-tì, ē-tàng thê-kiong thian-bûn ha̍k-ka kóo-kè sing-hē-thuân lāi-té oo-àm-bu̍t-tsit hun-pòo ê tsîng-hîng, mā ē-tàng thui-tshik hîng-tshinn tī tsit-kuá tsá-kî sing-hē lāi-té sī án-ná khai-sí hîng-sîng--ê.

[English] A Molten Galaxy Einstein Ring

It is difficult to hide a galaxy behind a cluster of galaxies. The closer cluster's gravity will act like a huge lens, pulling images of the distant galaxy around the sides and greatly distorting them. This is just the case observed in the featured image recently re-processed image from the Hubble Space Telescope. The cluster GAL-CLUS-022058c is composed of many galaxies and is lensing the image of a yellow-red background galaxy into arcs seen around the image center. Dubbed a molten Einstein ring for its unusual shape, four images of the same background galaxy have been identified. Typically, a foreground galaxy cluster can only create such smooth arcs if most of its mass is smoothly distributed -- and therefore not concentrated in the cluster galaxies visible. Analyzing the positions of these gravitational arcs gives astronomers a method to estimate the dark matter distribution in galaxy clusters, as well as infer when the stars in these early galaxies began to form. 藏踮

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