diff --git a/CHANGELOG.md b/CHANGELOG.md
index b6e8377..01713be 100644
--- a/CHANGELOG.md
+++ b/CHANGELOG.md
@@ -10,6 +10,11 @@ and this project adheres to [Semantic Versioning](https://semver.org/spec/v2.0.0
 
 ### Added
 
+- Added `kete.RectangleFOV.from_wcs`, allowing the construction of a FOV from a given
+  Astropy WCS object.
+- Added `kete.conversion.bin_data`, which allows for binning matrix data such as images.
+- Added tutorial showing precovery of an asteroid from a 1950's glass plate observation
+  done at the Palomar Observatory.
 - Added sunshield rotation calculation for NEO Surveyor.
 
 
diff --git a/docs/data/full_frame.png b/docs/data/full_frame.png
new file mode 100644
index 0000000..3089207
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diff --git a/docs/data/full_frame_annotated.png b/docs/data/full_frame_annotated.png
new file mode 100644
index 0000000..606fb1a
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diff --git a/docs/data/full_frame_annotated_zoom.png b/docs/data/full_frame_annotated_zoom.png
new file mode 100644
index 0000000..0fda942
Binary files /dev/null and b/docs/data/full_frame_annotated_zoom.png differ
diff --git a/docs/tutorials/index.rst b/docs/tutorials/index.rst
index 13302b3..b3c3f76 100644
--- a/docs/tutorials/index.rst
+++ b/docs/tutorials/index.rst
@@ -10,5 +10,6 @@ These are more in-depth worked examples.
    background
    propagation
    neatm
+   palomar
    kona
    wise
\ No newline at end of file
diff --git a/docs/tutorials/palomar.rst b/docs/tutorials/palomar.rst
new file mode 100644
index 0000000..6fe733a
--- /dev/null
+++ b/docs/tutorials/palomar.rst
@@ -0,0 +1,224 @@
+Palomar 1950 Plate
+==================
+
+Identification of an asteroid in a glass plate exposure from 1950 Palomar Mountain.
+
+Background
+----------
+
+On December 6th and 8th 1950, Rudolph Minkowski captured 2 long exposure images
+onto glass plates of the galaxy NGC2403 looking for time varying sources. On the
+cover slip for these plates was written "Asteroid", and an arrow was drawn on the
+plate identifying the streaking asteroid on the plates themselves. Details of the
+observations are included in
+`Tammann & Sandage (1968) <https://doi.org/10.1086/149487>`_ in their Table A1,
+although plate PH-98M is incorrectly listed as PH-98H (with the ending letter
+indicating the observer). These plates were exposed for approximately 30 minutes
+(although cloud cover reduced the exposure toward the end for one plate).
+
+These plates are stored at the Carnegie Science Observatories in Pasadena in their
+archives. One of Carnegie's Archivists, Kit Whitten, provided a scanned copy of
+the frames to Joe Masiero at CalTech IPAC around 2018. Masiero provided them for
+the following analysis.
+
+Here we will identify that asteroid which Minkowski captured over 70 years ago.
+
+
+Pre-processing
+--------------
+
+Some pre-processing was done on the scanned image before this analysis. First the
+data was binned by a factor of 8 in both axis to reduce the file size. Second it
+was passed to astrometry.net for a plate solution. This gives a valid WCS to work
+with, which is practically a requirement. Since the image was as scan of a
+film negative, it was also inverted.
+
+Limitations
+-----------
+
+- Astrometry.net is using the current star catalog, meaning if there are stars in
+  the field which have moved measurably, then the astrometry will be imperfect.
+- Observer position before 1972 is somewhat tricky to compute, and is currently not
+  well supported in Kete. This is a result of NASA NAIF (Navigation and Ancillary
+  Information Facility) only producing Earth orientation files back to about 1972.
+  This information can be calculated by other means with less precision, but this
+  is not currently implemented. As a result of this, the center of the Earth is used
+  as an approximation for the observers position, but this results in about an
+  arc-minute offset in calculated positions. Adding a better approximation of the
+  observer location shifts the results to sub PSF accuracy.
+- Record keeping of the exact time appears to be off by a few minutes, though this
+  may be an artifact of the observer position being approximate.
+
+
+FITs File
+---------
+
+First we load a FITs file, and grab frame information from its header.
+
+.. code-block:: python
+
+    import kete
+    import matplotlib.pyplot as plt
+    import numpy as np
+
+    from astropy.io import fits
+    from astropy.wcs import WCS
+
+
+    # load the fits file and associated WCS
+    frame = fits.open("data/19501206-NGC2403-reduced.fits.gz")[0]
+    wcs = WCS(frame.header)
+
+    # Time of observation, approximately 3 am local time
+    # Taken from table A1 of the paper cited above.
+    jd = kete.Time(2433622.977, scaling='utc').jd
+    
+    earth = kete.spice.get_state("Earth", jd)
+    fov = kete.fov.RectangleFOV.from_wcs(wcs, earth)
+
+    # Plot the frame
+    kete.irsa.plot_fits_image(frame)
+    plt.title("Dec 6 1950 - Palomar Mountain")
+    plt.tight_layout()
+    plt.savefig("data/full_frame.png")
+
+.. image:: ../data/full_frame.png
+   :alt: Raw frame scanned from the Dec 6 1950 plate.
+
+
+MPC Orbit Data
+--------------
+
+Next we must collect orbit information from the Minor Planet Center (MPC).
+We will load all known objects from their database, convert them to a kete State,
+and propagate those states to the epoch near the FITs file epoch we opened.
+
+We also trim out more distant and eccentric objects.
+
+.. code-block:: python
+
+    table = kete.mpc.fetch_known_orbit_data()
+    table = table[[str(t).isdigit() for t in table['desig']]]
+    table = table[table['ecc'] < 0.5]
+    table = table[table['peri_dist'] < 4]
+    states = kete.mpc.table_to_states(table)
+
+
+Quick Cut
+---------
+
+As we are only analyzing a single frame, and the speed of the object suggests it
+is not close to Earth, we can apply some approximations to remove many objects from
+contention.
+
+.. note::
+
+    This step below can be completely skipped, it is only an optimization to make the
+    orbit propagation faster. This step only really applies for off ecliptic field of
+    views, as any FOV on the ecliptic will already have most of the main belt as
+    possible objects.
+
+If we assume most objects stay in their orbital plane, but we simply don't know where
+they are along the plane, we can use the two body approximation to compute the plane's
+on sky position from the observers location.
+
+Here we assume that the object is likely a main belt, or main belt adjacent object,
+and in doing so we can assume an orbital period of between about 800 and 2500 days.
+
+If we sample the orbit 360 times around the period of 2500 days, objects with that period
+will be sampled at about 1 degree steps on the sky. We then check at each of these points
+how close the object came to the center of the FOV.
+
+.. code-block:: python
+    
+    # Define a convenience function to see how far the objects are from the FOV
+    def cur_angles(states, fov):
+        """
+        Given a list of states, compute how far they are from the center of a FOV
+        """
+        pointing = fov.pointing
+        angles = []
+        obs_pos = fov.observer.pos
+        for state in states:
+            vec = state.pos - obs_pos
+            angles.append(pointing.angle_between(vec))
+        return np.array(angles)
+
+    n_steps = 360
+    period = 2500
+
+    jd = np.median([s.jd for s in states])
+    states = kete.propagate_two_body(states, jd)
+    best = cur_angles(states, fov)
+
+    for dt in np.linspace(0, 1, n_steps) * period:
+        states = kete.propagate_two_body(states, jd + dt)
+        cur = cur_angles(states, fov)
+        best = np.min([best, cur], axis=0)
+    
+    mask = best < 3
+    print(f"Total of {sum(mask)} asteroids less than 3 degrees from the FOV")
+    states = kete.mpc.table_to_states(table[mask])
+
+::
+    
+    Total of 1148 asteroids less than 3 degrees from the FOV
+
+Exact Calculation
+-----------------
+
+Compute the visible states, including large main belt asteroids in the computation.
+For 1k objects this should take about a second.
+
+.. code-block:: python
+
+    vis = kete.fov_state_check(states, [fov], include_asteroids=True)[0]
+
+Results
+-------
+
+Plot the overlap of visible objects on the original frame.
+
+Two objects are possible, 382632 and 151109, however the second is off the edge of
+the glass plate itself so not visible.
+
+.. code-block:: python
+
+    wcs = kete.irsa.plot_fits_image(frame, percentiles=(40, 99))
+    for idx in range(len(vis)):
+        vec = vis.obs_vecs()[idx]
+        kete.irsa.annotate_plot(wcs, vec, style='o', px_gap=10, text=vis[idx].desig)
+    
+    plt.title("Dec 6 1950 - Annotated")
+    plt.savefig("data/full_frame_annotated.png")
+
+
+.. image:: ../data/full_frame_annotated.png
+   :alt: Frame with both objects annotated.
+
+
+Zoomed
+------
+
+Zooming in to the expected position of 382632, we see the original hand drawn arrow,
+along with correctly labeled streaking asteroid. Note the slight offset, which from
+analysis not performed here can be shown to be a result of our assumption that
+the observer is at the center of the Earth. A better assumption about observer
+position causes the alignment to match within the width of the blur.
+
+.. code-block:: python
+
+    wcs = kete.irsa.plot_fits_image(frame, percentiles=(30, 99.9))
+    kete.irsa.annotate_plot(wcs,
+                            vis.obs_vecs()[1],
+                            style='L',
+                            px_gap=5,
+                            length=10,
+                            text="    " + vis[1].desig)
+    kete.irsa.zoom_plot(wcs, vis.obs_vecs()[1])
+    plt.title(f"Dec 6 1950 - Annotated Zoom");
+    plt.savefig("data/full_frame_annotated_zoom.png")
+    plt.close()
+
+.. image:: ../data/full_frame_annotated_zoom.png
+   :alt: Zoom in of the expected object.
\ No newline at end of file
diff --git a/pyproject.toml b/pyproject.toml
index eda957e..a3721f5 100644
--- a/pyproject.toml
+++ b/pyproject.toml
@@ -48,6 +48,7 @@ docs = ["sphinx",
         "sphinx-gallery",
         "sphinx_rtd_theme",
         "click",
+        "pytz",
         ]
 
 # Options for pytest
diff --git a/src/kete/conversion.py b/src/kete/conversion.py
index 9e1d97a..03c80ef 100644
--- a/src/kete/conversion.py
+++ b/src/kete/conversion.py
@@ -195,6 +195,55 @@ def compute_tisserand(
     )
 
 
+def bin_data(data, bin_size=2, method="mean"):
+    """
+    Bin data, reducing the size of a matrix.
+
+    Parameters
+    ----------
+    data:
+        2 dimensional array of data to be reduced.
+    bin_size:
+        Binning size, binning of data is applied to both directions of the data.
+        If the bin size is not a multiple of the shape of the data, the data is
+        trimmed until it is.
+    method:
+        Which function is used to produce a single final value from the bins.
+        This includes 'mean', 'median', 'min', 'max'. NANs are ignored.
+    """
+    funcs = {
+        "mean": np.nanmean,
+        "median": np.nanmedian,
+        "min": np.nanmin,
+        "max": np.nanmax,
+    }
+
+    # dont trust the user, check inputs
+    if bin_size <= 0 or int(bin_size) != bin_size:
+        raise ValueError("Bin size must be larger than 0 and an integer.")
+    bin_size = int(bin_size)
+    if method not in funcs:
+        raise ValueError("'method' must be one of: ", list(funcs.keys()))
+
+    data = np.asarray(data)
+    if data.ndim != 2:
+        raise ValueError("Array must be 2 dimensional.")
+
+    xdim, ydim = data.shape
+    if xdim % bin_size != 0:
+        xdim = (xdim // bin_size) * bin_size
+        logger.warning("x dimension is not a multiple of bin size, trimming to size.")
+        data = data[:xdim, :]
+    if ydim % bin_size != 0:
+        ydim = (ydim // bin_size) * bin_size
+        logger.warning("y dimension is not a multiple of bin size, trimming to size.")
+        data = data[:, :ydim]
+
+    reshaped = data.reshape(xdim // bin_size, bin_size, ydim // bin_size, bin_size)
+
+    return funcs[method](funcs[method](reshaped, axis=1), axis=2)
+
+
 def dec_degrees_to_dms(dec: NDArray) -> Union[str, list[str]]:
     """
     Convert a declination in degrees to a "degrees arcminutes arcseconds" string.
diff --git a/src/kete/fov.py b/src/kete/fov.py
index 45adbf4..74fec4f 100644
--- a/src/kete/fov.py
+++ b/src/kete/fov.py
@@ -17,7 +17,7 @@
     fov_state_check,
     fov_spk_check as _fov_spk_check,
 )
-from .vector import State
+from .vector import State, Vector
 from . import spice
 
 
@@ -55,3 +55,30 @@ def fov_spice_check(desigs: list[str], fovs) -> list[State]:
     """
     obj_ids = [spice.name_lookup(n)[1] for n in desigs]
     return _fov_spk_check(obj_ids, fovs)
+
+
+def _from_wcs(wcs, obs: State) -> RectangleFOV:
+    """
+    Construct a RectangleFOV from an astropy WCS along with an observer state.
+
+    parameters
+    ----------
+    wcs:
+        An astropy WCS, this must include the shape of the array.
+    obs:
+        The observer position
+    """
+    types = wcs.axis_type_names
+    if types == ["RA", "DEC"]:
+        x, y = wcs.array_shape
+        corners = wcs.pixel_to_world_values([0, 0, x, x], [0, y, y, 0])
+        vecs = [Vector.from_ra_dec(ra, dec) for ra, dec in zip(*corners)]
+    else:
+        raise NotImplementedError(
+            f"Support for WCS with frame {types} is not currently supported."
+        )
+    return RectangleFOV.from_corners(vecs, obs)
+
+
+# Monkey patch the rust class with a new constructor.
+RectangleFOV.from_wcs = staticmethod(_from_wcs)
diff --git a/src/kete/rust/propagation.rs b/src/kete/rust/propagation.rs
index 0f1e1f0..99e4dbf 100644
--- a/src/kete/rust/propagation.rs
+++ b/src/kete/rust/propagation.rs
@@ -1,3 +1,4 @@
+use itertools::Itertools;
 use kete_core::{
     errors::Error,
     propagation::{self, moid, NonGravModel},
@@ -5,7 +6,6 @@ use kete_core::{
     state::State,
     time::{scales::TDB, Time},
 };
-use itertools::Itertools;
 use pyo3::{pyfunction, PyResult, Python};
 use rayon::prelude::*;
 
@@ -165,8 +165,9 @@ pub fn propagation_n_body_spk_py(
 ///
 /// This returns two lists of states:
 /// - First one contains the states of the objects at the end of the integration
-/// - Second contains the states of the planets at the end of the integration, which may
-///   be used as input for continuing the integration.
+/// - Second contains the states of the planets at the end of the integration.
+///
+/// The second set of states may be used as input for continuing the integration.
 ///
 /// Parameters
 /// ----------