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2004船尾座新星Nova Pup 2004


11月20日由日本冈山县津山市的Akihiko Tago茨城县水户市的Yukio Sakurai各自独立发现。

发现时亮度为7.6等(照像)和7.4等(CCD)。位置为赤经 07时 41分 53.76秒,赤纬 -27度 06分 36.9秒。

11月27日凌晨开始第一次观测。从天狼星出发到大犬DELTA,再到目标星。当时2点之后上中天,可以有几个月的观测时间。观测到2005年3月。

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光度变化:

2453336.255 8.11
2453337.271 8.36
2453359.188 9.56
2453366.171 10.08
2453371.158 10.49
2453375.142 10.40
2453375.146 10.50
2453377.174 10.26
2453379.184 10.45
2453384.144 10.27
2453391.121 10.60
2453402.127 10.75
2453421.056 11.22
2453427.067 11.16
2453442.070 11.75


2005年3月12日:


 

比较照片:

比较星图:

参考星:

编号 名称 星等
1 TYC6548-1531-1 8.66
2 TYC6548-976-1 7.88
3 TYC6548-71-1 7.84
4 TYC6548-707-1 10.64
5 TYC6548-1632-1 10.34
6 TYC6548-1488-1 10.49
7 TYC6548-1688-1 10.14
8 TYC6548-581-1 9.46
9 TYC6548-483-1 11.26
11 TYC6548-1776-1 10.74

拍摄方法:

FS78+LE30+995@31mm, B&W MODE, ISO400, NR, 16 or 30 sec

测量方法:

MATLAB:imnova.m:
测量距离最亮象素+/-R, 2R,3R,4R距离正方形内象素的和。(R=8)

察看星点取样:

EXCEL:nova.xls:
以4R减2R求出平均背景和噪声。在1R数据中去除噪声得出星像强度。假设背景强度反映了平场效应,将结果再除以噪声值。

MATLAB imnovamag.m:
假设图像的数据是线性的,拟合后求出新星亮度。

察看线性:


记事:

2004-11-27 2:07

三张照片和叠加照片分别测量。测量数据:

计算结果:

91:mag=8.0363
95:mag=8.602
92:mag=8.1195
叠加:mag=8.1108
其中图95 #4比较星数据明显异常,去除后mag=8.0711

2004-11-28 2:30

图片聚焦欠佳。使用叠加图片(30秒曝光)测量

噪声较大。

计算结果:mag=8.3662

2004-12-20 00:30

多日阴云之后天气晴好。测量2968和2968-2970三张叠加的nova3align。

计算结果分别为:

mag=9.4242

mag=9.5613

2004-12-27 0:07

天不甚晴,地平有薄云。正值满月,月光明亮。拍摄时找不到128M的卡,只好使用原配的8M卡,中间使用COM/USB线下载到计算机。

加测第9点 6548-453-1 11.26,线性符合不错:

计算结果:mag=10.088

2004-12-31 23:47

即将进入新的一年。天气晴好,但背景光稍亮。

计算结果:mag=10.49

2005-1-4 23:25/31

出现了预期中的亮度回升。测量2个点。加第11点为参考星。

2005-1-7 0:11

亮度继续回升

2005-1-9 0:25

亮度回落

2005-2-19

天光很亮。只用9等以下的恒星做比较

2005-2-25

聚焦不好。No.11作为No.10比较星。新星为No.11。用No.5-No.10的恒星做比较,线性很好。

2005-2-20

后处理。背景很强(月光)。数据误差较大。比较星同上。

2005-3-12

天气很好。1,2,3,6不做比较星。