ᴡʜᴀᴛ ᴀʀᴇ ᴛʜᴇ ᴘᴏssɪʙʟᴇ ᴇʀʀᴏʀs ᴛʜᴀᴛ ᴡᴇ ᴇɴᴄᴏᴜɴᴛᴇʀ ᴅᴜʀɪɴɢ ᴛʜᴇ ᴇsᴛɪᴍᴀᴛɪᴏɴ ᴏғ sᴛᴀʀ ғᴏʀᴍᴀᴛɪᴏɴ ʀᴀᴛᴇ?
Answers
Answer:
Kennicutt (1994) proposed a simplest formula to estimate star formation rate (SFR) of the galaxies. I want to calculate SFR of some dwarf galaxies using SDSS spectroscopy and compare it with the SFR model for star forming dwarfs.
I read some papers which highlighted that when using the Hα flux for SFR estimates, we encounter the following difficulties, which may cause systematic errors: (i) contamination by [NII] emission lines, close to the Hα line, (ii) contamination by the other Hα emitters (e.g, other emission nebulae, non-thermal emitters, such as active galactic nuclei (AGN)), and (iii) internal extinction.
On the other hand, it is said that SDSS spectra data are well calibrated, so we do not need to perform any further corrections.
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Answer:
how can thanks 2 time in 1 anwer
