Observed Spectral profile of Quasar 3C273
|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
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.
|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|
D= 3.26*v/H0 (million lt-yr)
(c: velocity of light, H0=70 km/s/Mpc)
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.