An astrophysicist working at an observatory is interested in finding clouds of hydrogen in the galaxy. usually, hydrogen is detected by looking for the balmer series of spectral lines in the visible spectrum. unfortunately, the instrument that detects hydrogen emission spectra at this particular observatory is not working very well and only detects spectra in the infrared region of electromagnetic radiation. therefore, the astrophysicist decides to check for hydrogen by looking at the paschen series, which produces spectral lines in the infrared part of the spectrum. the paschen series describes the wavelengths of light emitted by the decay of electrons from higher orbits to the n=3 level.
what wavelength λ should the astrophysicist look for to detect a transition of an electron from the n=7 to the n=3 level?
express your answer with the appropriate units.

For questions 1 and 2, consider the following experimental data.hydrogen emission lines were detected at the following wavelengths (in nm): 121.6102.697.395.093.8question 1use the electromagnetic radiation classifications below and figure 1-1 in the introductory information for this lab (in the lab manual) to determine the nf value for the experimental data provided? wavelength, ? (nm) 650 700 550 600 400 450 500 visible spectrum wavelength, ? (m) 11 10 3 10 10 10 8 10 5 10 10 -10 10 9 10 10 10 10 -12 10 microwave radio infrared x-ray ultraviolet gamma 1020 1019 1018 1 1016 015 1014 01 12 109108 frequency, v (hz)a.1b. 2c. 3d. 4e. 5question 2using the data for the emission line with the longest wavelength, the known value of nf (from question 1 in this prelab), and the value of ni (deduced from the ? and nf values) calculate the rydberg constant for hydrogen (rh) in units of m-1.a) 1.097 x 10-11 m-1b) 5.921 x 107 m-1c) 1.097 x 10-2 m-1d) 9.252 x 106 m-1e) 1.097 x 107 m-1