Re: 台灣 大溪天文台
Posted: 2023年9月04日(月) 21:26
大溪天文台 SN 2023ixf 超新星 光度測量和定位
SN 2023 ixf SuperNova Photometry and Astrometry by DaXi observatory。
Telescope: Celestron 14" SCT F/3.6
The focal length is 1288mm
Sampling CCD: American SBIG ST-10XME Total pixels: 3.2 megapixel, sensor pixels: 2184 x 1472 pixel pixel size: 6.8 micron, sensor size: 14.9 x 10.2mm.
Photoreceptor/system optical resolution: 1.1 arc sec/pixel resolution
Region: Taoyuan, Daxi, Taiwan. Typical light pollution area with Seeing Field =1.5 -2 arc sec. Star point sampling is performed under the night sky.
CHROMA V-Bessell:
CHROMA V-Bessell 大溪天文台採用測光度フィルター物語：
The highest quality filter for astronomical observation, using a high-quality optical glass substrate and a durable electron-sprayed hard-coat coating. All coatings are applied on the front, and stray light-absorbing anti-reflective coatings are on the back to prevent ghosting and maximize monochromatic light transmission.
It is extremely precise and precise, and its specific light transmission spectrum is stable and does not undergo wavelength shifts due to changes in temperature and humidity.
Figure 1: 2023 0714 SN2023ixf supernova three-color composite pseudo-color image
Figure 2: 2023 0714 SN 2023ixf supernova V band brightness measurement (GSC star chart system)
Figure 3: AAVSO(アメリカ変光星観測者協会) 2023 0714 latest data from Daxi Observatory and various observatories around the world SN 2023ixf supernova brightness curve changes
大溪天文台 TYGA TW code for AAVSO of world observer code 。
大溪天文台初步觀測 2023 SNixf 超新星的簡單報告和相關文獻:
Multiband Photometry Evolution in the First Weeks of SN 2023ixf
a possible II-L Subtype
Figure 3. The rise and the decline brightness decline of SN 2023ixf . The slope of the decrease in brightness of the observed
SNe is different in each color band, becoming steadily shallower as we move to redder wavelengths. For clarity, error bars are
not plotted The response differences seen in each filter applied to the observation of the supernova SN 2023ixf, led to an analysis
of the differences between photometric filters as ‘colour indexes”. This study focused on the comparison of B-V and
V-R indices, shown in Figure 4.
In Figure clearly appears a huge variation of the B-V colour indices during the first 50 days after explosion from
-0.20 ± 0.02 to +0.85 ± 0.02 and, similarly, V-R behaviour change from 0 ± 0.01 to +0.50 ± 0.01, presumably linked
to the cooling of the stellar photosphere.
Interestingly,the measurements show a point corresponding to May 25, 2023 (JD = 2460089.622) where B-V = V-R
= 0.024. Next, we see an increasing trend as would be expected from a hot blackbody which is cooling, to the extent
where most of the brightness in the B band has shifted towards the V and R bands .
由SN 2023ixf 的色指數研究的重點是B-V和V-R 兩色指數的比較，如圖所示。 在圖中，爆炸後的前50天，B-V 色指數明顯發生了巨大變化，從-0.20±0.02變化到+0.85±0.02! 類似地 V-R的變化曲線也從0±0.01變化到+0.50±0.01! 這可能與恒星爆發後的冷卻有關。 有趣的是，量測結果顯示了一個對應於2023年5月25日的點（JD=2460089.622），其中B-V=V-R=0.024 兩色指數曲線相交及反轉(b-v/v-r curve intersection and inversion)。 接下來，我們觀測到了一個新的趨勢，正如預期的那樣(possible II-L Subtype Supernova)
熱的黑體正在冷卻，B波段的大部分亮度已經向V和R波段轉移（Peebles 1965）。
大溪天文台在5月25,26,27日(JD2460090-2460092)開始觀測的連續三天也觀測到類似的兩色指數(B-V/V-R)曲線相交及反轉(b-v/v-r curve intersection and inversion).
#.SN2023 ixf 爆發後, 為 SN II Type超新星，其藍色光星等會逐漸地變暗。其曲線變化為最後一圖
天文學家理論認為， SNII -L的較線性曲線表現可能僅僅是因為SNII -L 的恆星氫氣包覆要小得多。
這次觀測SN2023 ixf 雖屬 II Type，但光度的變化還是早期階段，還是要靠未來段觀測才可判定是走II -P 還是II-L 曲線。
SN 2023ixf のカラー インデックス研究の焦点は、図に示すように、B-V および V-R カラー インデックスの比較です。 図では、爆発後の最初の 50 日間で、B-V カラー インデックスは明らかに -0.20±0.02 から +0.85±0.02 に劇的に変化しました! 同様に、V-R 変化曲線も 0±0.01 から +0.50±0.01 に変化しました!これは、星の爆発後の冷却に関係している可能性があります。 興味深いことに、測定結果は、2023 年 5 月 25 日 (JD=2460089.622)、B-V=V-R=0.024、2 色の指数関数曲線の交差および反転 (b-v/v-r 曲線の交差および反転) に対応する点を示しています。 次に、予想どおり、新しい傾向が観察されました (II-L 亜型超新星の可能性)
熱い黒体は冷却しており、B バンドの明るさの大部分は V バンドと R バンドに移行しています (Peebles 1965)。
大渓天文台も、5 月 25、26、27 日から 3 日間連続で、同様の 2 色指数 (B-V/V-R) 曲線の交差と反転 (b-v/v-r 曲線の交差と反転) を観測しました (JD2460090-2460092)。
#.SN2023 ixf 爆発後はSN II型超新星となり、青色の光の量は徐々に減っていきます。 曲線が最後の写真に変わります
天文学者らは、SNII-L のより直線的な曲線の挙動は単に SNII-L の恒星の水素エンベロープがはるかに小さいためである可能性があると理論付けています。
今回のSN2023 ixfの観測はタイプIIに属しますが、光度の変化はまだ初期段階にあり、II-Pに従うかII-Lに従うかは今後の観測に頼る必要があります。
This graph of the luminosity as a function of time shows the characteristic shapes of the light curves for a Type II-L and II-P supernova.
https://en.wikipedia.org/wiki/Type_II_supernova
Multiband Photometry and Spectral Evolution in the First Weeks of SN 2023ixf, a possible II-L Subtype Supernova
Multiband photometric observations and their evaluation to instrumental magnitudes were performed using standard Johnson-Cousins filters (B, V, Rc) as well r and g Sloan filters, and not standard ones (R, G, B, and Clear filters). These were recorded from 9 observatories and from the MicroObservatory Robotic Telescope Network. Additionally, low-resolution spectra of the Type II supernova SN 2023ixf were performed during the rise to the maximum brightness and the first 50 days after the maximum. The results describe the rapid ascent towards the maximum (2.5 magnitudes about in five days in the B filter) and the slow decrease after the maximum (0.0425 +/- 0.02 magnitudes/day in the B filter). The results highlight the strong variation of the B-V colour indices during the first 50 days (from -0.20 +/- 0.02 to +0.85 +/- 0.02) and V-R (from 0 +/- 0.01 to +0.50 +/- 0.01) after the explosion, presumably corresponding to the cooling of the stellar photosphere. Additionally, the presence of sharp H-alpha and H-beta lines with a strong P Cygni profile, indicate the existence of a gaseous envelope expanding away from the star. At 50 days after the explosion the magnitude decrease from the maximum was observed to continue where it faded by 2.5 magnitudes (B filter), thus we propose SN 2023ixf is a Type II, subtype L, supernova (SNe).
SN 2023 ixf SuperNova Photometry and Astrometry by DaXi observatory。
Telescope: Celestron 14" SCT F/3.6
The focal length is 1288mm
Sampling CCD: American SBIG ST-10XME Total pixels: 3.2 megapixel, sensor pixels: 2184 x 1472 pixel pixel size: 6.8 micron, sensor size: 14.9 x 10.2mm.
Photoreceptor/system optical resolution: 1.1 arc sec/pixel resolution
Region: Taoyuan, Daxi, Taiwan. Typical light pollution area with Seeing Field =1.5 -2 arc sec. Star point sampling is performed under the night sky.
CHROMA V-Bessell:
CHROMA V-Bessell 大溪天文台採用測光度フィルター物語：
The highest quality filter for astronomical observation, using a high-quality optical glass substrate and a durable electron-sprayed hard-coat coating. All coatings are applied on the front, and stray light-absorbing anti-reflective coatings are on the back to prevent ghosting and maximize monochromatic light transmission.
It is extremely precise and precise, and its specific light transmission spectrum is stable and does not undergo wavelength shifts due to changes in temperature and humidity.
Figure 1: 2023 0714 SN2023ixf supernova three-color composite pseudo-color image
Figure 2: 2023 0714 SN 2023ixf supernova V band brightness measurement (GSC star chart system)
Figure 3: AAVSO(アメリカ変光星観測者協会) 2023 0714 latest data from Daxi Observatory and various observatories around the world SN 2023ixf supernova brightness curve changes
大溪天文台 TYGA TW code for AAVSO of world observer code 。
大溪天文台初步觀測 2023 SNixf 超新星的簡單報告和相關文獻:
Multiband Photometry Evolution in the First Weeks of SN 2023ixf
a possible II-L Subtype
Figure 3. The rise and the decline brightness decline of SN 2023ixf . The slope of the decrease in brightness of the observed
SNe is different in each color band, becoming steadily shallower as we move to redder wavelengths. For clarity, error bars are
not plotted The response differences seen in each filter applied to the observation of the supernova SN 2023ixf, led to an analysis
of the differences between photometric filters as ‘colour indexes”. This study focused on the comparison of B-V and
V-R indices, shown in Figure 4.
In Figure clearly appears a huge variation of the B-V colour indices during the first 50 days after explosion from
-0.20 ± 0.02 to +0.85 ± 0.02 and, similarly, V-R behaviour change from 0 ± 0.01 to +0.50 ± 0.01, presumably linked
to the cooling of the stellar photosphere.
Interestingly,the measurements show a point corresponding to May 25, 2023 (JD = 2460089.622) where B-V = V-R
= 0.024. Next, we see an increasing trend as would be expected from a hot blackbody which is cooling, to the extent
where most of the brightness in the B band has shifted towards the V and R bands .
由SN 2023ixf 的色指數研究的重點是B-V和V-R 兩色指數的比較，如圖所示。 在圖中，爆炸後的前50天，B-V 色指數明顯發生了巨大變化，從-0.20±0.02變化到+0.85±0.02! 類似地 V-R的變化曲線也從0±0.01變化到+0.50±0.01! 這可能與恒星爆發後的冷卻有關。 有趣的是，量測結果顯示了一個對應於2023年5月25日的點（JD=2460089.622），其中B-V=V-R=0.024 兩色指數曲線相交及反轉(b-v/v-r curve intersection and inversion)。 接下來，我們觀測到了一個新的趨勢，正如預期的那樣(possible II-L Subtype Supernova)
熱的黑體正在冷卻，B波段的大部分亮度已經向V和R波段轉移（Peebles 1965）。
大溪天文台在5月25,26,27日(JD2460090-2460092)開始觀測的連續三天也觀測到類似的兩色指數(B-V/V-R)曲線相交及反轉(b-v/v-r curve intersection and inversion).
#.SN2023 ixf 爆發後, 為 SN II Type超新星，其藍色光星等會逐漸地變暗。其曲線變化為最後一圖
天文學家理論認為， SNII -L的較線性曲線表現可能僅僅是因為SNII -L 的恆星氫氣包覆要小得多。
這次觀測SN2023 ixf 雖屬 II Type，但光度的變化還是早期階段，還是要靠未來段觀測才可判定是走II -P 還是II-L 曲線。
SN 2023ixf のカラー インデックス研究の焦点は、図に示すように、B-V および V-R カラー インデックスの比較です。 図では、爆発後の最初の 50 日間で、B-V カラー インデックスは明らかに -0.20±0.02 から +0.85±0.02 に劇的に変化しました! 同様に、V-R 変化曲線も 0±0.01 から +0.50±0.01 に変化しました!これは、星の爆発後の冷却に関係している可能性があります。 興味深いことに、測定結果は、2023 年 5 月 25 日 (JD=2460089.622)、B-V=V-R=0.024、2 色の指数関数曲線の交差および反転 (b-v/v-r 曲線の交差および反転) に対応する点を示しています。 次に、予想どおり、新しい傾向が観察されました (II-L 亜型超新星の可能性)
熱い黒体は冷却しており、B バンドの明るさの大部分は V バンドと R バンドに移行しています (Peebles 1965)。
大渓天文台も、5 月 25、26、27 日から 3 日間連続で、同様の 2 色指数 (B-V/V-R) 曲線の交差と反転 (b-v/v-r 曲線の交差と反転) を観測しました (JD2460090-2460092)。
#.SN2023 ixf 爆発後はSN II型超新星となり、青色の光の量は徐々に減っていきます。 曲線が最後の写真に変わります
天文学者らは、SNII-L のより直線的な曲線の挙動は単に SNII-L の恒星の水素エンベロープがはるかに小さいためである可能性があると理論付けています。
今回のSN2023 ixfの観測はタイプIIに属しますが、光度の変化はまだ初期段階にあり、II-Pに従うかII-Lに従うかは今後の観測に頼る必要があります。
This graph of the luminosity as a function of time shows the characteristic shapes of the light curves for a Type II-L and II-P supernova.
https://en.wikipedia.org/wiki/Type_II_supernova
Multiband Photometry and Spectral Evolution in the First Weeks of SN 2023ixf, a possible II-L Subtype Supernova
Multiband photometric observations and their evaluation to instrumental magnitudes were performed using standard Johnson-Cousins filters (B, V, Rc) as well r and g Sloan filters, and not standard ones (R, G, B, and Clear filters). These were recorded from 9 observatories and from the MicroObservatory Robotic Telescope Network. Additionally, low-resolution spectra of the Type II supernova SN 2023ixf were performed during the rise to the maximum brightness and the first 50 days after the maximum. The results describe the rapid ascent towards the maximum (2.5 magnitudes about in five days in the B filter) and the slow decrease after the maximum (0.0425 +/- 0.02 magnitudes/day in the B filter). The results highlight the strong variation of the B-V colour indices during the first 50 days (from -0.20 +/- 0.02 to +0.85 +/- 0.02) and V-R (from 0 +/- 0.01 to +0.50 +/- 0.01) after the explosion, presumably corresponding to the cooling of the stellar photosphere. Additionally, the presence of sharp H-alpha and H-beta lines with a strong P Cygni profile, indicate the existence of a gaseous envelope expanding away from the star. At 50 days after the explosion the magnitude decrease from the maximum was observed to continue where it faded by 2.5 magnitudes (B filter), thus we propose SN 2023ixf is a Type II, subtype L, supernova (SNe).
