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Swift's Ultraviolet/Optical Telescope (UVOT)

For details of UVOT Data Analysis, see our Data Analysis page.

UVOT Rationale

Observations of GRBs have shown that optical afterglows typically decline in brightness as t-1.1 to t-2.1. Therefore, rapid response is required to observe these counterparts and determine their redshift while they are still bright. The UVOT is uniquely suited for afterglow studies. It has ultraviolet capability which is not possible from the ground, and it cannot be clouded out. It is also much more sensitive than any other quick reaction telescope. UVOT observations enable optimal ground-based observations by providing rapid optical images of the GRB field so that any optical or infrared counterpart can be quickly identified and studied. Stars in the FoV of the UVOT provide an astrometric grid for the GRB field.

Table 1. A basic description of the UVOT specifications.

Instrumentation Description
Telescope Modified Ritchey-Chrétien
Focal Ratio 12.7
Detector Intensified CCD
Detector Operation Photon Counting
Field of View 17 x 17 arcmin
Detection Element 2048 x 2048 pixels
Telescope PSF 2.5 arcsec @ 350 nm
Wavelength Range 170-650 nm
Filters 7
Sensitivity B = 22.3 in white light in 1000 s
Pixel Scale 0.502 arcsec
Brightness Limit v = 7.4 mag
Camera Speed 11 ms

UVOT GRB Observations

The UltraViolet and Optical Telescope (UVOT) is a diffraction-limited 30 cm (12" aperture) Ritchey-Chrétien reflector, sensitive to magnitude 22.3 in a 17 minute exposure. Table 1 and Figure 1 describe the basic specifications and layout of the instrument.

A schematic of the UVOT layout. See text below for details.

Figure 1. A schematic of the UVOT layout, which is a 30 cm Ritchie-Chrétien telescope. The path of light through the telescope is denoted by arrows. First the light travels through an open door down the baffle until it is redirected into the detector. The long baffle reduces stray light background. The detector sits in front of the detector power supply between two filter wheels. Behind the detector the processing electronics are housed in front of the telescopes power supply, which is connected to two separate Digital Electronics Modules, one prime the other redundant.

Immediately after a GRB is detected and located by the BAT, the spacecraft slews to point both the UVOT and the XRT at the GRB location. The spacecraft's ∼90 second time-to-target means that about 100 GRBs per year (about 1/3 of the total) are observed by the narrow field instruments during the gamma-ray emission.

When a new GRB is acquired by the spacecraft, the UVOT goes through a predetermined program of exposure times and filter combinations. The initial images are immediately sent to the ground for use as a finding chart by ground-based observers, and for comparison to archival observations of the same patch of sky to detect a variable source that could be the optical counterpart. The filtered observations give the temporal behavior as a function of wavelength. If the GRB has a redshift between z ∼ 1.3 and z ∼ 5, the filtered observations can also measure the photometric redshift of the GRB.

Optical image of a GRB afterglow, two days after it went off. See paragraph below for details.

Figure 2. Here is an optical image of a GRB afterglow two days after it went off. This observation was made using a large ground-based telescope (the 4.2 meter William Herschel Telescope, observation by Paul Groot) when the afterglow was around magnitude 20. This image is cropped to 2 arcminutes (compared to 17 arcmin for the UVOT FoV). The size of the 5 arcsecond diameter position determination from the XRT is shown as a green circle. The UVOT will be able to determine the location of any afterglow it sees to an accuracy of ∼0.5 arcsecond.

UVOT Technical Description

The UVOT design is illustrated in Figure 1. It is a 30 cm diameter modified Ritchey-Chrétien telescope with an f/2.0 primary that is re-imaged to f/13 by the secondary. This results in pixels that are 0.502 arcsec over its 17 arcmin square FoV. The filter wheel includes a 4-times magnifier that results in 0.13 arcsec pixels for near diffraction limited imaging. The optics used for Swift/UVOT are the flight spares from the XMM-Newton/Optical Monitor (OM). The telescope structure, baffle, and thermal designs are also from the XMM-Newton project.

UVOT filter wheel and detector.

Figure 3. UVOT Filter wheel assembly with detector.

The detectors are copies of two micro-channel plate intensified CCD (MIC) detectors from the XMM-Newton/OM design. They are photon counting devices capable of detecting very low signal levels, allowing the UVOT to detect faint objects over 170-650 nm. The design is able to operate in a photon counting mode, unaffected by CCD read noise and cosmic ray events on the CCD. The UVOT can autonomously determine the spacecraft drift using guide stars in the FOV. The UVOT design includes the XMM-Newton/OM 11 position filter wheel in front of the detectors. The two grisms can be used to obtain low resolution spectra of bursts brighter than approximately mb < 15.

UVOT Operation

Once Swift has slewed to a new burst, the UVOT acquires a 150 s white exposure of the target field. The 2x2 arcmin portion of the frame surrounding the XRT GRB position is compressed and telemetered to the ground within 50 s. The Swift Operations Center automatically posts this image to the GCN. During subsequent ground contacts, the full frame of the finding chart image is telemetered, as well as the observing sequence of image and event data for the suite of imaging and grism filters in the wheel. Images generally contain at least 15 serendipitous stars listed in existing astrometric catalogs, allowing sub-arcsec positioning. Unlike the XMM-Newton/OM, the UVOT autonomously reduces the high-voltage on the MCPs when bright (mB < 10) stars or Earthlight (25° of the limb) are in the FOV. This change removes the XMM-Newton requirement of preplanning UVOT observations. The UVOT can use a fast mode to produce high temporal resolution light curves (11 msec resolution).

UVOT Performance

The UVOT can detect a mB = 22.3 point source in 1000 s using the open (white) filter. A comparable 30 cm ground-based telescope is limited to 20th mag due to sky brightness and seeing. Given an mB = 22.3 source with a spectrum like an A0 star, the signal-to-noise ratio is ∼3 in 1000 s. Coincidence losses will start to degrade performance at count rates of greater than ∼10 count s-1 pixel-1.

Table 2. UVOT sensitivity limits. The counts are for an AOV star (Vega).

UVOT sensitivity: v = 20, in 1000 s gets:
v 143 counts
b 441 counts
u 217 counts
uvw1 99 cts
uvm2 53 counts
uvw2 87 counts
white 1306 counts
Sensitivity to Lymap-alpha cutoff
uvm2-uvw2 z ∼ 1.3
uvw1-uvm2 z ∼ 1.7
u-uvw1 z ∼ 2.3
b-u z ∼ 3.2
v-b z ∼ 5

The measured, on-orbit UVOT effective areas are shown below. The UVOT ultraviolet sensitivity is a significant improvement over the XMM-Newton/OM sensitivity. Second-order structure in the curves are governed by cubic spline interpolation over a small number of provided data points.

UVOT Broad Band Filters

UVOT broad band filter effective areas.

Figure 4. Effective area curves for the seven broadband UVOT filters shown as square centimeters versus wavelength in Angstroms. The white filter is shown in long dashed black. Dashed red--v, dashed black--b, dashed blue--u, solid red--uvw1, solid black--uvm2, solid blue--uvw2.

UVOT Grisms

Notes for observing with the UVOT visual Grism.

Notes for observing with the UVOT UV Grism.

Further Information

Further detail on the development and performance of the UVOT is available from the instrument teams: