The DDO photometric system1 It was developed at the David Dunlap Observatory near Toronto by McClure & van den Bergh (1968) It was developed at the David Dunlap Observatory near Toronto by McClure & van den Bergh (1968) Intermediate band system, filter defined: 48 (at λ4886), 45 (at λ4517), 42 (at λ4257), 41 (at λ4166), 38 b (at λ3815) and 35 (at λ3460) Intermediate band system, filter defined: 48 (at λ4886), 45 (at λ4517), 42 (at λ4257), 41 (at λ4166), 38 b (at λ3815) and 35 (at λ3460)

2 The DDO photometric system 210 stars, 70 star clusters and 56 galaxies were originally observed 210 stars, 70 star clusters and 56 galaxies were originally observed Purpose: measuring integrated light from galaxy nuclei and constructing stellar population models of galaxies and globular clusters  determining spectral types and luminosities of a wide range of reddened stars Purpose: measuring integrated light from galaxy nuclei and constructing stellar population models of galaxies and globular clusters  determining spectral types and luminosities of a wide range of reddened stars These observations were not originally intended to be the basis for a standard photometric system, but to supplement UBV-photometry by segregating stellar temperature and luminosity effects from reddening and ultraviolet excess These observations were not originally intended to be the basis for a standard photometric system, but to supplement UBV-photometry by segregating stellar temperature and luminosity effects from reddening and ultraviolet excess

The DDO photometric system3 System specifications and standard stars were revised by McClure (1975) because: System specifications and standard stars were revised by McClure (1975) because: –Many nights at Toronto were of dubious photometric quality (= large random errors), –Bandpass of the ultaviolet interference filter measuring line blanketing (38) was too narrow  limiting magnitude for observations of late-type stars was severely restricted –Only color indices were published (lack of a magnitude system difficults detection of variable stars) –Original Toronto filter set deteriorated shortly after observations were completed

The DDO photometric system4 New observations of 285 standard stars made on the 41- cm and 91-cm reflecting telescopes at Kitt Peak National Observatory ( ) replaced the original ones for the calculations New observations of 285 standard stars made on the 41- cm and 91-cm reflecting telescopes at Kitt Peak National Observatory ( ) replaced the original ones for the calculations Equipment used: conventional single channel photometers with dry-ice-cooled 1P21 photomultipliers Equipment used: conventional single channel photometers with dry-ice-cooled 1P21 photomultipliers Magnitude system for the 48 filter was incorporated (48M = V + 0,375 (B-V) for A-K stars) Magnitude system for the 48 filter was incorporated (48M = V + 0,375 (B-V) for A-K stars)

The DDO photometric system5 The DDO Filters (acc. McClure 1975) The DDO Filters (acc. McClure 1975) Specifications

The DDO photometric system6 The DDO Filters (acc. McClure 1975) The DDO Filters (acc. McClure 1975) Transmission curves

The DDO photometric system7 The DDO Filters (acc. McClure 1975) The DDO Filters (acc. McClure 1975) Transmissions of the standard DDO set

The DDO photometric system8 The DDO Filters (acc. McClure 1975) The following four filters have been used for Population I stars to provide measurementes of T eff, surface gravity and abundance of heavy elements: The following four filters have been used for Population I stars to provide measurementes of T eff, surface gravity and abundance of heavy elements: The 48 filter (λ4886): The 48 filter (λ4886): –Similar to the Hβ filter of Crawford & Mander, but its use here is not connected with the hydrogen line –Situated in a region of absorption by MgH The 45 filter bandpass (λ4517) : The 45 filter bandpass (λ4517) : –Situated in a region relatively free of strong spectral features –Comparison bandpass for the 42 and 48 filters

The DDO photometric system9 The DDO Filters (acc. McClure 1975) The 42 filter bandpass (λ4257) : The 42 filter bandpass (λ4257) : –Located shortward of the main CH absorption of the G band (λ4299) and longward of the violet cyanogen-band head (λ4216) The 41 filter bandpass (λ4166) : The 41 filter bandpass (λ4166) : –Located in the region of the violet cyanogen-band absorption

The DDO photometric system10 The DDO Filters (acc. McClure 1975) For very metal-poor Population II stars (weak or non-existent CN band) or where more than the abundance of CNO elements is of interest, metallic- line blanketing index are necessary: For very metal-poor Population II stars (weak or non-existent CN band) or where more than the abundance of CNO elements is of interest, metallic- line blanketing index are necessary: The 38b filter (λ3815) : The 38b filter (λ3815) : –Located shortward of the break near λ4000 (due to metallic blanketing in UV) The 35 filter (λ3460) : The 35 filter (λ3460) : –Identical to the “u” filter of Crawford & Barnes (1970) –Located shortward of the Balmer discontinuity and longward of the region where the Earth´s atmospheric absorption becomes total

The DDO photometric system11 The DDO Standard Stars (acc. McClure 1975) Almost all stars observed by McClure and van den Bergh (1968) were retained (about 2/3). Almost all stars observed by McClure and van den Bergh (1968) were retained (about 2/3). They were originally chosen acc. to following criteria: They were originally chosen acc. to following criteria: –Stars as bright as possible (to provide an easily observed set of standards) –Spectral type range from O9 to M6, including all luminosity classes –Both metal-poor and metal-rich stars –A number of unusual stars should be included (e.g. strong cyanogen absorption, peculiar, WR, metallic- lines, etc) –Half were picked to be brighter than 6.0mag, and half between 6.0 and 8.0 mag

The DDO photometric system12 The DDO Standard Stars (acc. McClure 1975) I t is always wise to limit the temperature range of standard stars observed. Most standards should be similar to the program stars in spectral type and luminosity class

The DDO photometric system13 The DDO Standard Stars (acc. McClure 1975) I t is always wise to limit the temperature range of standard stars observed. Most standards should be similar to the program stars in spectral type and luminosity class

The DDO photometric system14 The DDO color indices Succesive color indices are formed from measurements through each of the filter bandpasses. Succesive color indices are formed from measurements through each of the filter bandpasses. Example: for the intensity of light through filters 45 and 48  C(45-48) = 2,5 log (I48/I45) Example: for the intensity of light through filters 45 and 48  C(45-48) = 2,5 log (I48/I45) The C(45-48) index: The C(45-48) index: –Sensitivity to surface gravity for late-type stars (due to MgH absorption region for filter 48)

The DDO photometric system15 The DDO color indices The C(42-45) index: The C(42-45) index: - Designed to measure the break in the continuum of late-type stars due to the G band of CH and other nearby lines -The G band break is primarily sensitive to spectral type or Teff - Affected by microturbulence (in the 42 band CH lines presumably makes it more effective). The effect is stronger in coolest models and decreases with increasing Teff

The DDO photometric system16 The DDO color indices The C(41-42) index: The C(41-42) index: –Also called “cyanogen-index” –Sensitivity to luminosity (Lindblad, 1922) –Sensitivity to abundance of heavy elements (C, N)

The DDO photometric system17 The DDO color indices The C(38-42) index: The C(38-42) index: –Defined as [C(38-42) = C(38- 41)+C(41-42)] –Designed to be a blanketing index The C(35-38) index: The C(35-38) index: –Measures the Balmer discontinuity –Sensitive to both temperature and luminosity –Index of limited use for late stars (except for those too hot for C(45-48))

18 The DDO color-color diagrams The C(45-48) vs C(42-45) diagramm: The C(45-48) vs C(42-45) diagramm: –The most basic and important in the DDO system –It enables two-dimensional spectral classification as accurate as the MK-system –Central role in the determination of absolute magnitudes and metallicities of late-type Pop I giants when combined with the C(41-42) cyanogen index

The DDO photometric system19 The DDO color-color diagrams The C(41-42) vs C(42-45) diagramm: The C(41-42) vs C(42-45) diagramm: Very sensitive to overall metallicity (insofar as C and N vary in lockstep with Fe and the rest of the metals)

20 The DDO color-color diagrams The C(38-42) vs C(45-48) diagramm: The C(38-42) vs C(45-48) diagramm: Allows luminosity classification Allows luminosity classification

The DDO photometric system21 Impact of molecular absorption on DDO photometry DDO photometry measures a relatively narrow spectral window. It includes a number of strong molecular absorption features in late-type stars. It is interesting knowing the resulting color offsets relative to the original model for each molecule MgH, SiH, CH, CN DDO photometry measures a relatively narrow spectral window. It includes a number of strong molecular absorption features in late-type stars. It is interesting knowing the resulting color offsets relative to the original model for each molecule MgH, SiH, CH, CN

The DDO photometric system22 References McClure, Robert (1975), Standard Stars for DDO photometry, The Astronomical Journal, Vol 81, Nr. 3, p. 103 McClure, Robert (1975), Standard Stars for DDO photometry, The Astronomical Journal, Vol 81, Nr. 3, p. 103 Tripicco, M.J. and Bell, R.A. (1991), Exploring the properties of the DDO system using synthetic colors, The Astronomical Journal, Vol. 102, Nr. 2, p. 744 Tripicco, M.J. and Bell, R.A. (1991), Exploring the properties of the DDO system using synthetic colors, The Astronomical Journal, Vol. 102, Nr. 2, p. 744 McClure, R. and van den Bergh, S. (1968), Five-Color Intermediate-Band Photometry of Stars, Clusters and Galaxies, The Astronomical Journal, Vol 73, Nr. 5, Part 1, p. 313 McClure, R. and van den Bergh, S. (1968), Five-Color Intermediate-Band Photometry of Stars, Clusters and Galaxies, The Astronomical Journal, Vol 73, Nr. 5, Part 1, p. 313