| Date & Time: | Apr 13 2013, from 21:35 to 21:51 JST(+0900) |
| Composed 2 shots with 15 minutes exposed |
| Optical: | Meade 25cm(10") Schmidt Cassegrain (f=2500mm, F10.0) |
| with SBIG DSS7 Spectrometer |
| Auto-guided with Meade LX200 Equatorial & Pictor 201 XT |
| Cooled CCD Camera: | SBIG ST-402ME (Temp.: -25°C) |
| Location: | Ooizumi, Hokuto city, Yamanashi pref. |
Upper strip: taken spectrogram, Lower strip: stretched 3-pixel-width & pseudo-colored image
| Emission line | Hα | Hβ |
|---|
| Observed WL, λm | 7569.1 Å | 5627.8 Å |
| WL in literature, λ0 | 6562.9 Å | 4861.3 Å |
| Red shift, z | 0.1533 | 0.1577 |
| Recession velocity, v | 4.250×104 km/s | 4.361×104 km/s |
| Estimated distance, D | 1.979 bn. lt-yr | 2.031 bn. lt-yr |
| (average) | 2.005 bn. lt-yr |
|---|
z= (λm-λ0)/λ0
v= c*((1+z)2-1)/((1+z)2+1)
D= 3.26*v/H0 (million lt-yr)
(c: velocity of light, H0=70 km/s/Mpc)
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This page shows you the observed spectral profile of the Quasar 3C273 with an amateur-oriented spectrometer.
The vertical lines in a taken spectral strip are originated from emission lines of atoms and/or molecules in atmosphere and light pollution.
The profile has subtracted those influences.
The quasar has two clear emission lines of the Balmer series of hydrogen atoms, the H-alpha and the H-beta.
The wavelengths of both lines are shifted in longer side, have extraordinary large red shifts (z-values) exceeding 0.15.
A table in right has listed and indicated the estimated distance to the quasar from observed wavelengths.
The value can be calculated as about 2 billion light years under an assumption that the Hubble constant of H0 has 70 km/s/Mpc.
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