Scientific Calculations

Q: How are the Galactic extinction values calculated?
A: Galactic extinction is presented as total absorption Aλ in magnitudes, as calculated by three different methods.

  1. The first estimate of Galactic extinction uses the Schlafly & Finkbeiner (2011) recalibration of the Schlegel, Finkbeiner & Davis (1998; SFD98) extinction map based on dust emission measured by COBE/DIRBE and IRAS/ISSA. The recalibration assumes a Fitzpatrick (1999) reddening law with Rv = 3.1 and a different source spectrum than SFD98.

  2. The original SFD98 extinction values are also returned for comparison purposes. The individual values of the total absorption at each waveband are calculated from the list of A/E(B-V) in Table 6 of Schlegel, Finkbeiner & Davis (1998). We have adopted the standard Landolt UBVRI and SDSS ugriz filters for the optical total absorptions, and the UKIRT JHKL' filters for the near-infrared total absorptions. Please note that Schlegel et al. calculated the values of A/E(B-V) for these specific bandpasses using a spectral energy distribution for an elliptical galaxy. Therefore, the numbers displayed by NED for a specific object may not be appropriate for other closely related bandpasses or other galaxy types. The total absorptions are nominally consistent with an average R = A/E(B-V) = 3.1, but do not agree numerically with this average. See Appendix B of SFD98 and references therein for additional details.

    Note, too, the list of caveats in SFD98 Appendix C. In particular, they call attention to the areas within the Holmberg radii of LMC, SMC, and M31 -- total reddenings through these large galaxies are replaced by Galactic reddenings toward them. They also note that no contaminating sources at Galactic latitudes |b| < 5 degrees have been removed from their dust maps, so calculated reddenings at these low latitudes are especially uncertain and untrustworthy. They state that the formal uncertainty in normalizing the dust column density to the reddenings is 10%; this should probably be taken as a lower limit on the formal error of the calculated reddenings at |b| > 5 degrees.

    A few other galaxies may have unreliable Galactic extinction values as well. An example is M82 (see Johnson et al. 2009, Section 6.3) where emission by dust within the galaxy has apparently affected the Schlegel et al. estimate of the foreground Galactic extinction. We thank L. C. Johnson for alerting us to the M82 problem.

  3. The Burstein-Heiles total B-band absorption is given as AB = 4 E(B-V) + 0.005, consistent with AB = 4 E(B-V) in Burstein and Heiles (1984) and references therein but with a small adjustment to the zero point (Burstein, 1988, private communication). Burstein and Heiles used HI column densities combined with the Lick galaxy counts to determine the extinction for any object with |b| > 10 degrees (aside from a few small patches of sky where they had no HI data). South of -23 degrees, where the Lick counts stop, the Burstein/Heiles Galactic extinction estimates depend only on the HI column densities.

    We note that we have replaced the Burstein-Heiles extinction toward M31 with values that are not affected by the HI emission of M31 itself (see Burstein and Heiles 1984 for a discussion). This affects not only M31, but several thousand objects within that galaxy. Specifically, we have replaced "data word numbers" 402-405 in "physical record number" 20 in the Burstein-Heiles reddening file "redsouth.dat" with the E(B-V) values 0.068, 0.071, 0.074, and 0.077 (interpolated from surrounding areas), respectively. The original values were 0.043, 0.034, 0.024, and 0.045. (We thank Tod Lauer for alerting us to this problem.)

    One additional note: The zero points of these two reddening laws differ by 0.02 magnitudes in E(B-V), with Schlegel et al. adopting a higher zero point than Burstein and Heiles. (We thank David Burstein for this note.)

Willick (1999) adds the following notes and caution concerning the Galactic extinction calculations:
"Two all-sky Galactic extinction maps are presently available: the older Burstein-Heiles (Burstein and Heiles,ApJ 225, 40, 1978, hereafter BH, and AJ 87, 1165, 1982) maps, which are based on 21-cm column density and faint galaxy counts, and the more recently completed Schlegel, Finkbeiner, and Davis (ApJ 500, 525, 1998, hereafter SFD) maps, based on IRAS/DIRBE measurements of diffuse IR emission. The SFD extinctions have been favored in several recent analyses and, indeed, were used in Paper I (Willick, ApJ 516, 47, 1999). Unlike BH, the SFD extinctions are based directly on dust emission and have comparatively high spatial resolution. However, it has not been established beyond doubt that they are free of systematic errors, such as could arise from the presence of cold dust invisible to IRAS. The BH extinctions are also vulnerable to possible systematic effects, such as a variable dust-to-gas ratio and galaxy count fluctuations. Thus, it seems prudent to use both methods, or linear combinations of them, and see what effect this has on the results."

Q: How are the coordinates for NED objects chosen?
A: We try to adopt the best published position for each object. In many cases, this will be the position in the catalog in which the object originally appeared: IRAS sources originally had positions from the IRAS PSC or FSC, NVSS sources originally had positions from NVSS, and so forth.

Because NED's source hierarchy is based on physical models for the sources, we try to use optical positions for sources associated with galaxies, clusters, and so on. However, if a galaxy, for example, is known to be associated with a compact nuclear radio source, and if a better position at a radio wavelength is available, we will adopt the radio position. Similarly, if an IRAS source is identified with a galaxy, and if an accurate optical position is available for that galaxy, we will choose the optical coordinates in preference to the IRAS position.

We are continually updating NED's positions as better coordinates are measured and published. We also measure positions (primarily from the Digitized Sky Survey) to help sort out problem areas of the sky, or to resolve discrepant published positions.

Q: Is there an easy way to precess my coordinates?
A: NED offers an easy-to-use coordinate calculator. This provides coordinate transformation, precession, and position angle calculations, as well as Schlegel et al. Galactic extinction. The coordinate calculator is flexible enough to convert accurately between Besselian and Julian equinoxes, taking the epoch of observation into account when needed. It assumes that Besselian dates refer to FK4 system, that Julian dates refer to the FK5 system, and makes the appropriate transformations.

Q: What precession routine has NED adopted?
A: NED adopted the FK5 system in 1992 with J2000.0 as the default equinox. The precession routine is essentially that described in the introduction to FK5, with minor changes to support the work then being done at IPAC. J. Bennett, the author of the routine, has provided an extensive description of NED's precession calculations. Though NED does not yet explicitly support the International Celestial Reference Frame (ICRF), the FK5 optical system is consistent with ICRF to within the known errors of the FK5 system (see e.g., Ma et al. 1998).

Q: Is there an easy way to change coordinate systems?
A: NED's coordinate calculator (see the previous question) will handle transformation from one coordinate system to another. It currently handles transformations among the ecliptic, equatorial, Galactic, and supergalactic coordinate systems.

Q: What kind of magnitude is listed in the Basic Data?
A: These are usually optical magnitudes taken from the astronomical literature, and should be understood as being indicative only. We are adding letters after the magnitudes indicating the band pass to which the magnitude applies. For example, we use "U", "B", "V", "R", and "I" for the standard Johnson and/or Cousins magnitudes in the optical; "p" for photographic magnitudes from e.g. IIa-O or 103a-O plates, "g" for Gunn g-band magnitudes, "j" for magnitudes from III-aJ plates, "J" for 2MASS near-IR magnitudes, and so on.

We will eventually have all of NED's Basic Data magnitudes flagged with the band passes. In the meantime, the magnitude may have already been included in NED's table of of referenced Photometric Data.

Q: What are the sources for the photometric data in NED?
A: Most of NED's detailed photometric data are taken from the larger catalogs, though we have also loaded many shorter lists from the journals as well. The Basic Data for each object, displayed on the Object Search Results pages, are from heterogeneous unreferenced sources, typically measured in the optical or near-infrared part of the spectrum (see the previous question). The data displayed on the Photometric Data Search Results pages are fully referenced. These data may apply to any part of the spectrum from gamma rays to radio.

Q: Have the photometric data in NED been transformed or reduced in any way?
A: NED displays its collection of detailed photometry in two ways. First, the "data as published" and enough information to understand and use them are given. Then, NED applies the appropriate flux conversion factor, if needed, to reduce the published data to a common set of MKS units: W/m2/Hz (1 Jy = 10-26 W/m2/Hz).

NED has adopted effective wavelengths, band widths, and absolute calibrations for the different photometric systems from the papers containing the data, or from the papers originally defining the photometric systems. If this information is not given in the original papers, we have assumed the values in this table.

Q: Why are there negative fluxes and flux densities in NED?
A: NED attempts to represent the published literature as accurately as possible. Sometimes this will lead us to include negative fluxes and flux densities, and/or measurement errors larger than the detections themselves. In these cases, we encourage you to read the original papers to check the validity of the flux and flux density values.

Q: What kind of redshifts are used in NED?
A: We use heliocentric redshifts. When we display them as velocities, we use the optical convention Vsun = czsun. Note that we do not make any relativistic correction to these velocities. John Huchra at the Harvard-Smithsonian Center for Astrophysics has kindly supplied more information on the definition of extragalactic redshifts.

Q: Some of the reported redshifts in NED seem to show discrepancies with my estimates. Why?
A: As with the celestial coordinates which we adopt for the objects in NED, we attempt to use the best available redshifts. However, occasional errors creep into NED, in spite of our best efforts. If you find one of these cases, please let us know so that we can fix NED and document the origin of the error.

Q: Is there any information which explains the jargon used in the photometry of objects in NED?
A: As with the redshifts, we encourage you to go back to the original paper to fully understand the magnitudes adopted by NED.

Here are a few examples of magnitudes currently found in NED's detailed photometric data:

  • u, g, r, i, or z usually refers to the five-band SDSS photometric system
  • B is a B-band magnitude on the Johnson system
  • BT is a total magnitude in the B-band
  • BT0 is a total magnitude in the B-band corrected to "face-on" (i.e. inclination = 0 degrees)
  • bj is approximately a B magnitude derived from photometry on a IIIa-J plate
  • R25 is an R magnitude at the 25th mag arcsec-2 isophote level
  • J, H, or Ks usually refers to the three-band 2MASS photometic system