In astronomy Westerhout 49 also known as W49, is a strong galactic thermal radio source characteristic of an HII region. It was discovered by Gart Westerhout in 1958. Its distance is estimated to be about 11.1 kpcs or 36,000 light years. and it lies in the galactic plane about the same distance from the galactic centre as does the Sun. It has been compared to the giant HII region NGC 3603 which is about half as distant. Non-thermal radiation has been found which is believed to be from an old supernova remnant. Gaseous molecular outflows have been detected as well as H2O (water) masers . No optical counterpart has yet been discovered. While this is partly due to interstellar absorption, any tight clustering of stars at such a great distance in the galactic plane would be scarcely distinguis
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| - Westerhout 49 (es)
- Westerhout 49 (en)
- 韋斯特豪特49 (zh)
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| - Westerhout 49 (también conocida cómo W49) es una fuente de ondas de radio con propiedades similares a la de una región HII, situada en la constelación del Águila y descubierta por el astrónomo Gart Westerhout en 1958. Su distancia al Sol se estima en alrededor de 11,4 kilopársecs (37000 años luz). Está tan lejos que el polvo interestelar la hace invisible en el óptico, por lo que para su estudio hay que recurrir a otras longitudes de onda además de las ondas de radio, cómo por ejemplo el infrarrojo, que penetran en él. (es)
- 韋斯特豪特49也稱為W49，是銀河系的一個有著強熱電波源特徵的氫離子區。它是在1958年發現的。 它的距離估計約為11,100秒差距或36,000光年。它位於銀河系平面上，與銀河系中心的距離大約與太陽相同。與巨大的氫離子區NGC 3603比較，其距離只有6,900秒差距。已經發現的非熱輻射，被認為是來自一個古老的超新星殘骸，也已經檢測到氣態分子流出以及H2O（水）邁射，但尚未發現光學對應物。雖然這部分是由於星際吸收，但在銀河系平面上如此遠距離的任何恆星緊密聚集，一般都與背景幾乎沒有區別。 2014年發表的一項研究，使用了VLT與其它儀器，表明在這個恆星形成區域的中心星團中存在一顆非常大的恆星。所述恆星的參數（“W49nr1，也稱為[WBB2016] 1”）到目前為止的約束性很差，但是估計的光度是太陽的幾百萬倍，初始質量在100到180太陽質量之間，甚至可能更多。因此將它列入最亮和質量最大的恆星表中。位於該區的另一顆恆星，[WBB2016] 2，質量為250太陽質量，也是已知最明亮和質量最大的恆星之一。 (zh)
- In astronomy Westerhout 49 also known as W49, is a strong galactic thermal radio source characteristic of an HII region. It was discovered by Gart Westerhout in 1958. Its distance is estimated to be about 11.1 kpcs or 36,000 light years. and it lies in the galactic plane about the same distance from the galactic centre as does the Sun. It has been compared to the giant HII region NGC 3603 which is about half as distant. Non-thermal radiation has been found which is believed to be from an old supernova remnant. Gaseous molecular outflows have been detected as well as H2O (water) masers . No optical counterpart has yet been discovered. While this is partly due to interstellar absorption, any tight clustering of stars at such a great distance in the galactic plane would be scarcely distinguis (en)
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| - UKIDSS JHK image of W49 (en)
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| - Westerhout 49 (también conocida cómo W49) es una fuente de ondas de radio con propiedades similares a la de una región HII, situada en la constelación del Águila y descubierta por el astrónomo Gart Westerhout en 1958. Su distancia al Sol se estima en alrededor de 11,4 kilopársecs (37000 años luz). Está tan lejos que el polvo interestelar la hace invisible en el óptico, por lo que para su estudio hay que recurrir a otras longitudes de onda además de las ondas de radio, cómo por ejemplo el infrarrojo, que penetran en él. (es)
- In astronomy Westerhout 49 also known as W49, is a strong galactic thermal radio source characteristic of an HII region. It was discovered by Gart Westerhout in 1958. Its distance is estimated to be about 11.1 kpcs or 36,000 light years. and it lies in the galactic plane about the same distance from the galactic centre as does the Sun. It has been compared to the giant HII region NGC 3603 which is about half as distant. Non-thermal radiation has been found which is believed to be from an old supernova remnant. Gaseous molecular outflows have been detected as well as H2O (water) masers . No optical counterpart has yet been discovered. While this is partly due to interstellar absorption, any tight clustering of stars at such a great distance in the galactic plane would be scarcely distinguishable from the general background. A study published in 2014, where the VLT has been used among other instruments, shows the presence of a very massive star in the central cluster of this star-forming region. The parameters of said star (W49nr1, also known as [WBB2016] 1) are so far poorly constrained, but a luminosity of several million times that of the Sun is estimated as well as an initial mass between 100 and 180 solar masses, and perhaps even more, what would place it among both the most luminous and massive stars known. Another star located in the region, [WBB2016] 2, has a mass of 250 solar masses, and is also one of the most luminous and massive stars known. (en)
- 韋斯特豪特49也稱為W49，是銀河系的一個有著強熱電波源特徵的氫離子區。它是在1958年發現的。 它的距離估計約為11,100秒差距或36,000光年。它位於銀河系平面上，與銀河系中心的距離大約與太陽相同。與巨大的氫離子區NGC 3603比較，其距離只有6,900秒差距。已經發現的非熱輻射，被認為是來自一個古老的超新星殘骸，也已經檢測到氣態分子流出以及H2O（水）邁射，但尚未發現光學對應物。雖然這部分是由於星際吸收，但在銀河系平面上如此遠距離的任何恆星緊密聚集，一般都與背景幾乎沒有區別。 2014年發表的一項研究，使用了VLT與其它儀器，表明在這個恆星形成區域的中心星團中存在一顆非常大的恆星。所述恆星的參數（“W49nr1，也稱為[WBB2016] 1”）到目前為止的約束性很差，但是估計的光度是太陽的幾百萬倍，初始質量在100到180太陽質量之間，甚至可能更多。因此將它列入最亮和質量最大的恆星表中。位於該區的另一顆恆星，[WBB2016] 2，質量為250太陽質量，也是已知最明亮和質量最大的恆星之一。 (zh)
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