diff --git a/specsim/data/config/desiY1.yaml b/specsim/data/config/desiY1.yaml
deleted file mode 100644
index ca4e709..0000000
--- a/specsim/data/config/desiY1.yaml
+++ /dev/null
@@ -1,384 +0,0 @@
-name: DESI QuickSim
-
-# The base path is pre-pended to all non-absolute path values below.
-# {...} will be expanded using environment variables.
-base_path: '{DESIMODEL}/data'
-
-# Be verbose during the simulation?
-verbose: no
-
-# Specify the wavelength grid to use for simulation. For comparison, the
-# table below summarizes the ranges of non-zero throughput in each camera,
-# wavelengths that can disperse into CCDs (with a 5-sigma cut), and the
-# extents of each CCD's active pixels covered by all fibers (as defined by
-# cameras.*.ccd.table below). Note that individual fibers will generally have
-# slightly more coverage, so we are simulating the worst-case coverage of
-# all fibers.
-#
-#   Range     b(min)   b(max)   r(min)   r(max)   z(min)   z(max)
-#            Angstrom Angstrom Angstrom Angstrom Angstrom Angstrom
-# ---------- -------- -------- -------- -------- -------- --------
-# Throughput 3533.000 5998.000 5564.000 7805.000 7360.000 9913.000
-# Simulation 3550.000 ................................... 9850.000
-#   Response 3565.400 5952.600 5621.700 7744.300 7431.000 9838.000
-#        CCD 3569.000 5949.000 5625.000 7741.000 7435.000 9834.000
-wavelength_grid:
-    unit: Angstrom
-    min: 3550.05
-    max: 9850.05
-    step: 0.1
-
-# The atmosphere configuration is interpreted and validated by the
-# specsim.atmosphere module.
-atmosphere:
-    # Sky emission surface brightness.
-    sky:
-        table:
-            # The .dat extension is not automatically recognized as ascii.
-            format: ascii
-            columns:
-                wavelength: { index: 0, unit: Angstrom }
-                surface_brightness:
-                    index: 1
-                    # Note the factor of 1e-17 in the units!
-                    unit: 1e-17 erg / (Angstrom arcsec2 cm2 s)
-            paths:
-                # Each path defines a possible condition.
-                dark: spectra/spec-sky.dat
-                grey: spectra/spec-sky-grey.dat
-                bright: spectra/spec-sky-bright.dat
-        # Specify the current condition.
-        condition: dark
-    # Atmospheric seeing (only used when instrument.fiberloss.method = galsim)
-    seeing:
-        # The seeing is assumed to scale with wavelength as
-        # fwhm(wlen) = fwhm_ref * (wlen / wlen_ref) ** -0.2
-        fwhm_ref: 1.1 arcsec
-        wlen_ref: 6355 Angstrom
-        # The seeing PSF is modeled as a Moffat profile.
-        moffat_beta: 3.5
-    # Surface brightness of scattered moonlight.
-    moon:
-        # Un-normalized spectrum of scattered moonlight.
-        # We use the Wehrli 1985 extraterrestial solar spectrum here.
-        # Seee http://rredc.nrel.gov/solar/spectra/am0/ for details.
-        table:
-            columns:
-                wavelength: { index: 1, unit: Angstrom }
-                flux:
-                    index: 2
-                    # The actual units are W / (m2 micron) but we lie here
-                    # (by a factor of 10) since the input normalization does
-                    # not matter and old versions of speclite.filters do
-                    # not interpret the actual units correctly.
-                    unit: erg / (cm2 s Angstrom)
-            path: sky/solarspec.txt
-            format: ascii.basic
-        constants:
-            # Phase of the moon from 0 (full) to 1 (new).
-            moon_phase: 0.5
-            # Zenith angles of the moon. An angle > 90 (below the horizon)
-            # will zero the scattered moon contribution.
-            moon_zenith: 100 deg
-            # Separation angle between the observation and moon.
-            separation_angle: 60 deg
-    # Zenith extinction coefficients.
-    extinction:
-        table:
-            format: ascii
-            columns:
-                wavelength: { index: 0, unit: Angstrom }
-                extinction_coefficient: { index: 1 }
-            path: spectra/ZenithExtinction-KPNO.dat
-    # Should extinction be applied to the sky emission?
-    extinct_emission: yes
-    # Airmass to use when the pointing is not calculated from the source
-    # and observation parameters. The focal_x and focal_y parameters of
-    # source.location.constants must be set in order for the airmass
-    # specified here to be used.
-    airmass: 1.0
-
-# The instrument configuration is interpreted and validated by the
-# specsim.instrument module.
-instrument:
-    # See DESI documents 334, 336, 347 for details.
-    name: DESI
-    constants:
-        # These values are copied from desimodel/data/desi.yaml
-        primary_mirror_diameter: 3.797 m
-        obscuration_diameter: 1.8 m
-        support_width: 0.03 m
-        fiber_diameter: 107.0 um
-        field_radius: 414.0 mm
-    plate_scale:
-        table:
-            path: focalplane/platescale.txt
-            format: ascii
-            columns:
-                radius: { index: 0, unit: mm }
-                radial_scale: { index: 6, unit: um/arcsec }
-                azimuthal_scale: { index: 7, unit: um/arcsec }
-    fiberloss:
-        # Method for calculating fiberloss fractions.
-        # Either galsim or table or fastsim.
-        method: fastsim
-        # Number of wavelengths where fiberloss should be calculated
-        # and interpolated. Ignored unless method is galsim.
-        num_wlen: 11
-        # Number of pixels used to subdivide the fiber diameter for
-        # numerical convolution and integration calculations with galsim.
-        num_pixels: 16
-        # Table of pre-tabulated fiberloss fractions vs wavelength for
-        # different source types.  Ignored unless method is table.
-        table:
-            format: ascii
-            paths:
-                # Each path corresponds to a different source type.
-                qso: throughput/fiberloss-qso.dat
-                elg: throughput/fiberloss-elg.dat
-                lrg: throughput/fiberloss-lrg.dat
-                star: throughput/fiberloss-star.dat
-                sky: throughput/fiberloss-sky.dat
-                perfect: throughput/fiberloss-perfect.dat
-            columns:
-                wavelength: { index: 0, unit: Angstrom }
-                fiber_acceptance: { index: 1 }
-        # Fits file of precomputed galsim fiber acceptances.
-        # Ignored unless method is fastsim.
-        # The fits file is created with specsim/fitgalsim.py
-        # and used by specsim/fastfiberacceptance.py
-        # Comment out this line to disable the "fastsim" mode (e.g., if
-        # this file is not available or describes a different config).
-        fast_fiber_acceptance_path: throughput/galsim-fiber-acceptance.fits
-    blur:
-        # Read RMS blur values tabulated as a function of field angle and
-        # wavelength, and derived from ray tracing simulations.  For details,
-        # see $DESIMODEL/doc/nb/DESI-0347_Throughput.ipynb.
-        path: throughput/DESI-0347_blur.ecsv
-        # The ECSV format is not auto-detected so we specify it explicitly.
-        format: ascii.ecsv
-    offset:
-        # Read radial centroid offsets tabulated as a function of field angle
-        # and wavelength, and derived from ray tracing simulations.  For
-        # details, see $DESIMODEL/doc/nb/DESI-0347_Throughput.ipynb.
-        path: throughput/DESI-0347_offset.ecsv
-        # The ECSV format is not auto-detected so we specify it explicitly.
-        format: ascii.ecsv
-        #
-        # static/stable achromatic but correlated centroid offsets from a FITS file
-        # this is to emulate any systematic residual of the plate maker
-        # in particular the effect of the corrector lens
-        # polishing errors (see DESI-1071)
-        # DESI-0347_static_offset_*.fits is the worst case scenario where
-        # we cannot correct for this during commissionning
-        # Uncomment any one of these lines to select a different random set.
-        # If all lines are commented out, this effect is ignored.
-        #static: throughput/DESI-0347_static_offset_1.fits
-        #static: throughput/DESI-0347_static_offset_2.fits
-        #static: throughput/DESI-0347_static_offset_3.fits
-        #
-        # random achromatic and uncorrelated offsets with 1D rms = sigma1d
-        # ( per axis, i.e. sqrt(mean(dx**2+dy**2))=sqrt(2)*sigma1d )
-        # this is to emulate an uncorrelated positionner, astrometric, ... errors
-        # see lateral error in DESI-347 which is the throughput budget spreadsheet
-        #
-        # in DESI-347-v11 the quadratic sum of all lateral error terms except
-        # 'Band-limited chromatic shift microns' (already included in radial centroid offsets)
-        # and 'FVC corrector optics figure error' (a static term)
-        # is 7.38 um = 5.22 * sqrt(2) um
-        sigma1d: 5.22 um
-        # Random offsets are generated independently for each fiber of each exposure,
-        # but reproducibly according to this seed.
-        seed: 123
-    cameras:
-        b:
-            constants:
-                # These values are copied from desimodel/data/desi.yaml
-                read_noise: 3.29 electron/pixel**2
-                # We treat "pixel" as a linear unit, so we need pixel**2 here.
-                dark_current: 1.89 electron/(hour pixel**2)
-                gain: 1.0 electron/adu
-                # Clip the resolution matrix at this number of sigmas.
-                num_sigmas_clip: 5
-                # Output pixels are used to report simulation results but are
-                # not the physical pixels.  The output pixel size must be a
-                # multiple of wavelength_grid.step.
-                output_pixel_size: 0.8 Angstrom
-            ccd:
-                table:
-                    path: specpsf/psf-quicksim-rebin.fits
-                    hdu: QUICKSIM-B
-                    extrapolated_value: 0.0
-                    columns:
-                        wavelength: { name: wavelength }
-                        row_size:
-                            name: angstroms_per_row
-                            # The file uses Angstrom / row but "row" is not
-                            # recognized by astropy.units so we replace it with
-                            # the linear "pixel" unit.
-                            unit: Angstrom / pixel
-                            override_unit: yes
-                        fwhm_resolution: { name: fwhm_wave }
-                        neff_spatial: { name: neff_spatial }
-            throughput:
-                table:
-                    path: throughput/thru-b_y1measured.fits
-                    hdu: THROUGHPUT
-                    extrapolated_value: 0.0
-                    columns:
-                        wavelength: { name: wavelength, unit: Angstrom }
-                        throughput: { name: throughput }
-        r:
-            constants:
-                # These values are copied from desimodel/data/desi.yaml
-                read_noise: 2.69 electron/pixel**2
-                # We treat "pixel" as a linear unit, so we need pixel**2 here.
-                dark_current: 1.14 electron/(hour pixel**2)
-                gain: 1.0 electron/adu
-                # Clip the resolution matrix at this number of sigmas.
-                num_sigmas_clip: 5
-                # Output pixels are used to report simulation results but are
-                # not the physical pixels.  The output pixel size must be a
-                # multiple of wavelength_grid.step.
-                output_pixel_size: 0.8 Angstrom
-            ccd:
-                table:
-                    path: specpsf/psf-quicksim-rebin.fits
-                    hdu: QUICKSIM-R
-                    extrapolated_value: 0.0
-                    columns:
-                        wavelength: { name: wavelength }
-                        row_size:
-                            name: angstroms_per_row
-                            # The file uses Angstrom / row but "row" is not
-                            # recognized by astropy.units so we replace it with
-                            # the linear "pixel" unit.
-                            unit: Angstrom / pixel
-                            override_unit: yes
-                        fwhm_resolution: { name: fwhm_wave }
-                        neff_spatial: { name: neff_spatial }
-            throughput:
-                table:
-                    path: throughput/thru-r_y1measured.fits
-                    hdu: THROUGHPUT
-                    extrapolated_value: 0.0
-                    columns:
-                        wavelength: { name: wavelength, unit: Angstrom }
-                        throughput: { name: throughput }
-        z:
-            constants:
-                # These values are copied from desimodel/data/desi.yaml
-                read_noise: 2.69 electron/pixel**2
-                # We treat "pixel" as a linear unit, so we need pixel**2 here.
-                dark_current: 1.14 electron/(hour pixel**2)
-                gain: 1.0 electron/adu
-                # Clip the resolution matrix at this number of sigmas.
-                num_sigmas_clip: 5
-                # Output pixels are used to report simulation results but are
-                # not the physical pixels.  The output pixel size must be a
-                # multiple of wavelength_grid.step.
-                output_pixel_size: 0.8 Angstrom
-            ccd:
-                table:
-                    path: specpsf/psf-quicksim-rebin.fits
-                    hdu: QUICKSIM-Z
-                    extrapolated_value: 0.0
-                    columns:
-                        wavelength: { name: wavelength }
-                        row_size:
-                            name: angstroms_per_row
-                            # The file uses Angstrom / row but "row" is not
-                            # recognized by astropy.units so we replace it with
-                            # the linear "pixel" unit.
-                            unit: Angstrom / pixel
-                            override_unit: yes
-                        fwhm_resolution: { name: fwhm_wave }
-                        neff_spatial: { name: neff_spatial }
-            throughput:
-                table:
-                    path: throughput/thru-z_y1measured.fits
-                    hdu: THROUGHPUT
-                    extrapolated_value: 0.0
-                    columns:
-                        wavelength: { name: wavelength, unit: Angstrom }
-                        throughput: { name: throughput }
-
-# The source configuration is interpreted and validated by the
-# specsim.source module.
-source:
-    name: 22nd AB magnitude reference
-    # The type is only used when instrument.fiberloss.method is 'table'.
-    type: qso
-    table:
-        format: ascii
-        path: spectra/spec-ABmag22.0.dat
-        columns:
-            wavelength: { index: 0, unit: Angstrom }
-            flux:
-                index: 1
-                # Note the factor of 1e-17 in the units!
-                unit: 1e-17 erg / (Angstrom cm2 s)
-    # Transverse profile of the source on the sky, used to calculate the
-    # fiberloss fraction when instrument.fiberloss.method = galsim (but
-    # ignored otherwise).
-    profile:
-        # The sum of disk + bulge fractions must be <= 1. If it is < 1,
-        # the remainder is point-like, i.e., star or QSO.
-        disk_fraction: 0.0
-        bulge_fraction: 0.0
-        disk_shape:
-            half_light_radius: 0.8 arcsec
-            position_angle: 45 deg
-            minor_major_axis_ratio: 0.5
-        bulge_shape:
-            half_light_radius: 1.2 arcsec
-            position_angle: 60 deg
-            minor_major_axis_ratio: 0.8
-    # Location of the source on the sky. A source will not be visible if
-    # it lies out the observation field of view.
-    location:
-        # If focal-plane (x,y) coordinates are not specified, they will be
-        # calculated from the sky coordinates and observing conditions
-        # and the corresponding airmass will be used for the atmosphere model.
-        constants:
-            # Comment out these lines to have (x,y) and the airmass
-            # calculated automatically for this source and observation.
-            focal_x: -70.7 mm
-            focal_y: +70.7 mm
-        # Sky coordinates are optional (and ignored) when focal-plane (x,y)
-        # are specified.
-        sky: { coordinates: 0h 0d, frame: icrs }
-    # Set these parameters to apply a redshift transformation.
-    z_in:
-    z_out:
-    # Set these parameters to normalize in a specified filter.
-    filter_name:
-    ab_magnitude_out:
-
-# The observation configuration is interpreted and validated by the
-# specsim.observation module.
-observation:
-    observatory: KPNO
-    constants:
-        exposure_time: 1000.0 s
-        # Atmospheric pressure at the telescope (not at sea level) used
-        # to calculate atmospheric refraction.  Leave commented out to use a
-        # nominal value calculated for the observatory elevation.
-        #pressure: 79 kPa
-        # Air temperature at the telescope used to calculate atmospheric
-        # refraction (but only has a small effect).
-        temperature: 15 deg_C
-        # Relative humidity (0-1) at the telescope used to calculate atmospheric
-        # refraction (but only has a small effect).
-        relative_humidity: 0.
-    exposure_start:
-        timestamp:
-            when: 55000.5
-            format: mjd
-        # This optional parameter adjusts the timestamp by +/-12h to
-        # achieve the specified hour angle for the boresight (ra, dec).
-        #adjust_to_hour_angle: -0.5h
-    pointing:
-        sky:
-            coordinates: 0h 0d
-            frame: icrs