4 Additional photometric systems

The 17 new photometric systems added to the ADPS are here briefly noted. The wavelength and width of the bands listed in this section (including terminology and number of decimal figures) are those given in the original papers, while wavelengths and widths given in the rest of this paper (electronic Figs. 9-187) come from our computations based on the actual band profiles. The new systems with available band transmission profiles are:

Strömgren and Gyldenkerne - 1955 (Fig. 15). From a series of 25 interference filters with transmission peaks in the range 3800-5500 Å  used to measure 110 MKK standard stars at the Observatoire de Haute-Provence, a first group of four filters was isolated and used by Strömgren (1956) to define his uvby system aiming to study F stars (and later extended to A and B types). A second group of five filters was selected by Strömgren & Gyldenkerne (1955) to become the base of a system designed to measure G and K stars, in particular the CaII-K line, the discontinuity at the G-band and CN intensity. The adopted bands have widths at half maximum of 100 Å and central wavelengths at 3910, 4030, 4170, 4240 and 4360 Å.

Bahner - 1963 (Fig. 31). A system composed by 16 square bands in the range 3200-6400 Å aimed to investigate B and A stars. Four bands are devoted to the measurement of the Balmer continuum, and ten bands to the optical continuum away from strong absorption features.

Mould and Wallis - 1977 (Fig. 103). In ADPS I we briefly mentioned it as a modification of the Mould - 1976 system. Actually, the differences are large enough to justify its inclusion in ADPS II as a separate photometric system. It is aimed to the measurement of CaH and TiO bands in M stars and T Tau stars of the M spectral type. Five bands, realized with interference filters, have their central wavelengths (and widths at half maximum) at 5450 (200), 6940 (140), 7140 (140), 7520 (140) and 8500 (400) Å.

Malyuto et al. - 1997 (Fig. 142). This is a system with six sets of bands, each one composed by three square bands, aimed to quantitatively classify K and M stars via the strengh of FeI (+TiO $\alpha_1$) around 5013, Mgb (+TiO $\alpha_0$) at 5235, NaI D (+TiO  $\gamma_{1}^{\prime}$) at 5930, TiO  $\gamma_{0}$ at 7235, TiO  $\gamma_{0}^{\prime}$ 6250 and TiO  $\gamma_{1}$ 6723 Å bands. The bands are realized on spectra and are found to be insensitive to differences in data reduction procedures, reddening and resolution of the spectral catalogues to which they are applied. The system is claimed to provide an average accuracy of 0.6 spectral subtype and 0.8 luminosity class in the classification of K and M stars.

Hickson and Mulrooney - 1998 (Fig. 145). A survey of 20 deg² in 33 narrow bands complete to mag $\sim$20 has been conducted with the 3-m liquid mirror telescope of the NASA Orbital Debris Observatory. The filters have central wavelengths ranging from 4545 to 9477 Å, at intervals of $\sim$0.01 in $\lg \lambda$, and give a resolving power of $\lambda/\Delta\lambda \sim44$. The survey aims to provide photometric redshifts of $\sim$10⁴ galaxies and QSOs and accurate photometry and spectral classification for $\sim$10⁴ field stars. Central wavelengths (and bandwidths) of the photometric bands (in Å) are: 4545 (177), 4659 (185), 4756 (193), 4860 (202), 4981 (219), 5102 (224), 5190 (227), 5327 (228), 5451 (210), 5570 (214), 5711 (217), 5856 (231), 5976 (243), 6137 (236), 6287 (264), 6411 (240), 6546 (280), 6713 (291), 6880 (292), 7044 (299), 7187 (306), 7347 (322), 7524 (332), 7696 (319), 7875 (333), 8059 (346), 8248 (337), 8438 (356), 8679 (351), 8831 (413), 9063 (353), 9245 (400) and 9477 (391).

JHK KPNO - Manduca and Bell - 1979 (Fig. 162). The transmission of the JHK filters in use at KPNO are given together with local Earth's atmosphere transmission. KAO far-IR - Harvey - 1979 (Fig. 163). This is the five bands, far-IR photometric system for the He-cooled bolometer attached to the 0.91 m telescope on board the Kuiper Airborne Observatory airplane. The bolometer explores the range of wavelengths blocked by the Earth's atmosphere longward of 35 $\mu$m. The $\lambda_{\rm eff}$ and widths at half maximum (for a Sun-like energy distribution as reflected by a planetary surface) of the five bands are (in $\mu$m): 40 and 31-49 (band KAO-40); 52 and 44-59 (KAO-52); 100 and 80-130 (KAO-100N); 110 and 80-155 (KAO-100B); 160 and 125-250 (KAO-160).

IRTS FIRP - Lange et al. - 1994 (Fig. 173). The Far-IR Photometer (FIRP) on the IR Telescope in Space (IRTS) provided absolute photometry in four bands, whose central wavelengths (and widths at half maximum) are: 150 (68), 250 (135), 400 (130) and 700 (370) $\mu$m. S-520-15 FIR - Matsuhara et al. - 1994 (Fig. 174). A five bands, far-IR photometer was placed aboard a S-520-15 rocket launched on Feb. 2, 1992 by ISAS (Japan) from the Kagoshima Space Center. The He-cooled telescope aimed to the detection of diffuse far-IR emission at high galactic latitudes during the 350 s flight outside the atmosphere. It carried both wide bands (BC1, BC2 and BC3) and narrow ones, the latter's goal being the detection of diffuse emission in the [CII] line at 157.7 $\mu$m (a narrow LC band at the line nominal wavelength, and an associated control CC band on the adjacent continuum). The central wavelengths and widths at half maximum of the bands are (in $\mu$m): 95 and 19 (band BC1); 134 and 13 (BC2); 186 and 23 (BC3); 157.9 and 1.3 (LC); 153.7 and 1.5 (CC).

iz, iJ, iH, iK, iL, iL$^\prime$, iM, in, iN, iQ - Young et al. - 1994 (Fig. 177). It is the optimization of infrared bands by Young et al. (1994) in response to recommendations made by the Working Group on Infrared Extinction and Standardization of IAU Commission 25. The optimization aims to enhance reproducibility and trasformability and to allow the use of linear extinction curves by reducing the effect of molecular absorption at the edges of the photometric bands. Peak weavelengths and widths at half maximum are (in $\mu$m): 1.032 and 0.073 (band iz); 1.240 and 0.079 (iJ); 1.628 and 0.152 (iH); 2.196 and 0.188 (iK); 3.620 and 0.274 (iL); 3.900 and 0.274 ($iL^\prime$); 4.675 and 0.114 (iM); 9.030 and 0.323 (in); 11.10 and 2.00 (iN); 17.90 and 1.61 (iQ).

ABU SPIREX - 1998 (Fig. 181). A six band photometric system is available at the 60-cm telescope of the SPIREX facility at the South Pole, operated by the Center for Astrophysical Research in Antartica (CARA) and NOAO (Fowler et al. 1998 and http://www.noao.edu/scopes/south_pole/). The bands have their central wavelength and width at half-maximum as follow (in $\mu$m): 2.4245 and 2.4076-2.4414 (band H₂Q(3)); 3.299 and 3.262-3.336 (PAH); 3.514 and 3.205-3.823 (L); 3.821 and 3.520-4.122 (L$^\prime$); 4.051 and 4.024-4.078 (Br$\alpha$); 4.668 and 4.586-4.749 (M_N).

JHK$^\prime$K_sKL$^\prime$M$^\prime$   MKO - Tokunaga et al. - 2002 (Fig. 182). The new set of near-IR filters for the Mauna Kea Observatories (MKO) is designed to avoid as much as possible the detrimental effects of telluric absorption bands, to the aim of reducing background noise, improving photometric transformations between Observatories, providing greater accuracy in extrapolating to zero airmass, and reducing the color dependence of extinction coefficients. The central wavelengths and widths at half maximum (in $\mu$m) for the seven bands are (Tokunaga et al. 2002): 1.250 and 1.170-1.330 (band J); 1.635 and 1.490-1.780 (H); 2.120 and 1.950-2.290 ($K^\prime$); 2.150 and 1.990-2.310 ($K_{\rm s}$); 2.200 and 2.030-2.370 (K); 3.770 and 3.420-4.120 ($L^\prime$); 4.680 and 4.570-4.790 ($M^\prime$).

The new systems censed in the ADPS that have no documentation about their band transmission profiles (and that are therefore not further considered in this paper) are:

Aerobee IR-65 - 1965. An Aerobee rocket carrying a N₂-cooled telescope was launched on Oct 29, 1965 for a scan of the sky during a $\sim$300 s ballistic flight outside the atmosphere. Two photometric bands were realized: InAs with a band-pass from 1 to 3 $\mu$m and AuGe with a band-pass from 3 to 7 $\mu$m (McNutt et al. 1966; Harwit et al. 1966).

DIRBE COBE - Kelsall et al. - 1990. DIRBE is an absolute photometer on COBE (COsmic Background Explorer). It is internally stabilized to 1% repeatibility and it is equipped with 10 infrared bands. They are the J(1.25 $\mu$m), K(2.3), L(3.5) and M(4.5) bands, plus the IRAS bands nominally at 12, 25, 60 and 100 $\mu$m, and two additional bands at 160 and 240 $\mu$m.

SpaceLab IRT - Kent et al. - 1992. Survey scans of the sky at six infrared wavelengths were obtained with IRT (infrared telescope experiment), as part of the SpaceLab-2 mission on the Space Shuttle 51-F. The six bands have width at half maximum (in $\mu$m) of 1.7-3.0, 4.5-9.5, 6.1-7.1, 8.5-14, 18-30 and 70-120. Data collected at $\lambda > 3~\mu$m were corrupted by the high background radiation generated by the Shuttle environment. Data from the shortest band were instead useful in producing a map of the Galaxy emission at 2.4 $\mu$m. The single-band photometric system is defined by the flux of three reference stars (g Her, $\alpha$ Her and $\mu$ Cep).

MSX - Egan and Price - 1996. The infrared telescope radiometer (SPIRIT III) aboard the Ballistic Missile Defense Organization (BMDO) Mid-course Space Experiment (MSX) has been used to pinpoint infrared astrometric reference stars (177 860 sources cataloged, Egan & Price 1996). The radiometer includes six photometric bands whose mean wavelengths and widths at half maximum are (in $\mu$m): 4.29 and 4.22-4.36 (band B₁); 4.35 and 4.24-4.46 (B₂); 8.26 and 6.0-10.9 (A); 12.1 and 11.1-13.2 (C); 14.7 and 13.5-16.0 (D); 21.4 and 18.1-26.0 (E).

TIRCAM 2 - Persi et al. - 2002. Mid-IR photometric system for the TIRGO Infrared Observatory, defined by the flux at 1.0 airmass of six reference stars ($\alpha$ Lyr, $\beta$ Gem, $\alpha$ Boo, $\beta$ And, $\beta$ Peg and $\alpha$ Tau) as given in Persi et al. (2002). $\lambda_{\rm eff}$ and widths at half maximum are (in $\mu$m): 8.81 and 8.4-9.2 (band F[8.8]); 9.80 and 9.3-10.3 (F[9.8]); 10.27 and 9.8-10.8 (F[10.3]); 11.69 and 11.1-12.3 (F[11.7]); 12.49 and 11.9-13.1 ([F12.5]). The TIRCAM 2 is an upgrade of a previous TIRCAM 1 (Persi et al. 1996) version.