|Space Telescope Science Institute|
|WFC3 Instrument Handbook|
7.5.1 Filter and Grism SummaryAn overview of the IR spectral elements and of the process by which they were selected was given in Section 2.3. This section gives details of the IR filters and grisms. Table 7.2 lists the IR channel’s filters, with a general description and fundamental parameters of each. Figures 7.2 and 7.3 show the effective throughput curves, including the filter transmission multiplied by the throughput of the OTA, WFC3 optics, and detector response.More detailed information on the throughput curves of all of the filters is given in Appendix A:WFC3 Filter Throughputs; in particular, Section A.2.1 describes how to generate tabular versions of the throughput curves using synphot. All measurements of the IR filters which involve wavelengths, as tabulated in Table 7.2 and plotted in Figures 7.2 and 7.3 and in Appendix A:WFC3 Filter Throughputs, were done in helium rather than vacuum. It should be noted that the laboratory measurements were done at a temperature of –30°C, whereas the filters are operated on orbit at –35°C; this may lead to wavelength shifts which are expected to be very small.The IR channel is equipped with a single filter wheel with 18 slots, containing 15 passband filters, two grisms, and an opaque element (also referred to as the BLANK) for dark current measurements. The filter complement samples the spectral region between 800 and 1700 nm. All of the IR filter elements are full-sized, covering the entire field of view of the IR detector. Since all of the elements are mounted in a single wheel, only one element can be used at a given time.The 900–1700 nm wavelength range is covered by a series of wide- and medium-band filters, with little wavelength overlap. Additional medium-band filters are centered on molecular bands and nearby continua, and several narrow-band filters are available for probing interstellar and nebular recombination lines.The filter set is designed to include the most popular passbands used in extragalactic, stellar, and solar-system astronomy, as well as passbands similar to those already used in previous HST instruments.Table 7.2: WFC3 IR Channel Filters and Grisms.
Name1 Pivot2 λp
Wide Y Wide YJ Wide J Wide JH gap; red grism reference WFC3 H H2O/CH4 continuum H2O/CH4 line H2O and NH3 Paschen β Paschen β continuum Paschen β (redshifted) Useful range: 800–1150 nm4
“Pivot wavelength” is defined as in Table 6.2 and Section 9.3. Filter transmissions were measured in helium but have been converted to vacuum wavelengths for this table.
Figure 7.2: Integrated system throughput of the WFC3 IR wide-band filters, presented in two panels for clarity. The throughput calculations include the HST OTA, WFC3 IR-channel internal throughput, filter transmittance, and the QE of the IR detector.Figure 7.3: Integrated system throughput of the WFC3 IR medium-band filters (top panel) and narrow-band filters (bottom panel). The throughput calculations include the HST OTA, WFC3 IR-channel internal throughput, filter transmittance, and the QE of the IR detector.The IR channel’s versions of the ground-based J and H filters are F125W and F160W, respectively. The F125W filter has a width somewhat wider than that of a typical J passband used in ground-based cameras. The F160W filter’s bandpass has been modified relative to ground-based H in order to give a better fit to the QE curve of the IR detector. Specifically, the WFC3 H filter’s bandpass has been narrowed to approximately 1400-1700 nm, in order to limit thermal background and to have the filter define the bandpass on the red side rather than the detector sensitivity cutoff. By contrast, NICMOS H filter (NICMOS F160W) covers about 1400-1800 nm. This narrowing for WFC3 reduces photometric errors due to spatial variations in the detector’s QE cutoff.The wide F140W filter covers the gap between the J and H bands that is inaccessible from the ground. F105W has a central wavelength similar to ground-based Y, but is considerably wider. The IR channel also includes a very wide filter, F110W, spanning the ground-based Y and J bands. This filter can be used for deep imaging, with a bandpass fairly similar to that of the corresponding wide-band filter in NICMOS (also called F110W).The F098M filter is useful as the G102 grism reference, allowing source selection and wavelength zero-point determination. It also complements the UVIS F845M filter, whose red 50% critical wavelength is ~900 nm. The overlap allows coverage over a continuous wavelength range across both WFC3 detectors.The other medium filters span absorption bands of water and methane (F139M) and water and ammonia (F153M), with an adjacent continuum filter (F127M). These filters were intended for compositional studies of planets searching for water vapor (WFC3 ISR 2000-09). Solar system objects with visible inventories of these gas species are too bright to observe with the medium-band filters, and WFC3 lacks occulting hardware to access the high contrast ratios and small angular separations that would enable direct imaging of exoplanets. However, the high sensitivity of WFC3 enables compositional studies of the atmospheres of cool stars, brown dwarfs, and transiting exoplanets with the medium-band filters.The IR channel includes six narrow-band filters which sample some of the most astrophysically important planetary, stellar, and nebular spectral features in the near-IR (e.g., [Fe II] and Paschen-β).Cosmological emission lines can be detected across a range of redshifts within the bandpasses of the narrow-band filters. Table 7.3 lists the redshifts that can be probed using the specified emission lines. These redshift ranges are offered as a guide; exact values depend on the wavelengths of the filter cutoffs. Filter cutoffs used in Table 7.3 were defined using the passband rectangular widths (defined in 4 of Table 6.2). For consistency with Table , passband cutoffs were not centered on the filter pivot wavelengths λp (defined in Section 9.3). Instead, a central wavelength for each filter was determined by maximizing the wavelength-integrated product of a rectangular passband of the specified width with the actual system throughput for the filter. For the IR narrow-band filters, these rectangular passband equivalent central wavelengths are within 0.3% of the pivot wavelengths.
Filter λp (nm) Minimum cz (km/sec) Maximum cz (km/sec) Pa β on or [Fe II] off z (Pa β) or Pa β off [Fe II] off or Pa β off The IR channel has two grisms that provide slitless spectra (see Chapter 8 for more details). The “blue” G102 grism provides a dispersion of 2.5 nm/pix (or a resolution of ~210) over the 800-1150 nm wavelength range. The “red” G141 grism has a dispersion of 4.7 nm/pix (resolution of ~130) over the 1100-1700 nm range. In most cases, a grism observation will be accompanied by a direct image, for source identification and wavelength calibration (see Section 8.3).7.5.2 Filter Blue LeaksAll of the IR filters have been constructed using IR-transmitting colored glass with thin-film coatings to achieve the desired bandpasses. As with the UVIS filter designs, better in-band transmission generally means somewhat less suppression of out-of-band transmission. While the final IR filters have excellent in-band transmission (>90%), a few also have a small, narrow peak of transmission between 750-800 nm. After the filters were manufactured, a new IR detector was chosen which has appreciable sensitivity well down into the optical wavelength range (see Figure 5.18). Some of the IR filters thus have a small amount of blue leak (i.e., a small amount of short-wavelength out-of-band light is detected). None of the IR filters have significant red leaks.Table 7.4 presents estimates of the blue-leak effect, listing the fraction of detected count rate expected from 710 to 830 nm for each filter. The throughput calculation includes transmission of the filter, the throughputs of the HST OTA and the IR optics, and the QE of the IR detector.As can be seen from the table, blue leaks in all the wide-band and some of the narrow- and medium-band filters are minimal; however, several filters, notably F126N, F128N, and F153M, have some blue leak (e.g., ~1% for objects with effective temperatures of 5000 K.) In programs that may suffer adverse effects due to the blue leaks, it may be useful to obtain UVIS images in the F763M filter, which covers the problematic wavelength region (750-800 nm).Table 7.4: Fraction of detected count rate arising between wavelengths 710 to 830 nm as a function of effective temperature.
Teff (K) 7.5.3 Ghosts