Changes resulting from the NVSS flux corrections

The corrections in NVSS fluxes leading to the corrected Version 1.1 also result in changes to some of the figures and tables in Kimball & Ivezić (2008). The results are qualitatively the same. However, there are some changes in published numbers, such as population percentages and model fits. These are reported below. The new versions of the figures, along with the original versions (in high resolution), are available here.

Changes in numbers reported in the text

The original value of each number is shown in parentheses.

Section 3.5.1. NVSS Sources Without a FIRST Counterpart

For the sample of NVSS detections brighter than 18 mJy, we now find that 0.54% (0.43%) lack both FIRST and WENSS counterparts. Above 12 mJy, we find that 1.8% (2.3%) of NVSS sources have no FIRST match.

Section 4.4.1. Spectroscopically-Identified Quasars

With regards to the lower left panel in Figure 19: a Kolomogorov-Smirnov test rejects the null hypothesis that the two histograms share the same parent distribution at the 99.2% (99.6%) level.

Figures

Figures 6 and 7: The distributions are more sharply centered around t_FIRST - t_NVSS = 0. (These figures, along with Table 4, continue to motivate Δt = 0.35 as the optimal separator between "simple" and "complex" sources).

Figures 9, 11, 16: Some changes in percentages of objects reported in each class.

Figures 20 and 21: Changes in percentages of objects reported in each class, as well as steeper values of the radio spectral slope evident.

All other figures showed no qualitative or significant quantitative changes.

Tables

Table 3: Parameters Describing Model Fits (Sum of Two Gaussians) to the Distributions of Δt Shown in the Lower Panel of Figure 6

Bin	Simple Sources			Complex Sources
Bin	Fraction	Mean	σ	Fraction	Mean	σ
t_NVSS < 12	0.71	0.0054	0.042	0.29	0.55	0.34
12 < t_NVSS < 13	0.69	0.020	0.068	0.31	0.59	0.36
13 < t_NVSS < 14	0.67	0.030	0.11	0.33	0.62	0.45
14 < t_NVSS < 15	0.68	0.061	0.19	0.32	0.52	0.47

Table 4: Results of Automatic and Visual Morphology Classification for a Set of 1071 Radio Quasars and Radio Galaxies (Identified Spectroscopically from the SDSS)

Visual classification is listed at the left; automatic classification is listed along the top.

Visual classification	Total		Complex (%)		Resolved (%)		Compact (%)
Visual classification	QSOs	Gals.	QSOs	Gals.	QSOs	Gals.	QSOs	Gals.
Complex	202	286	75	94	9	5	16	1
Resolved	87	79	6	42	75	58	19	0
Compact	278	144	3	22	9	28	88	50

Table 5: The Sky Density, Mean, Median, and FWHM of the Average Spectral Index Histograms Shown in Figure 14

Subclass	deg^-2	Mean	Median	FWHM
Complex
All	1.30	-0.869	-0.864	0.432
no SDSS	1.10	-0.886	-0.881	0.407
galaxy	0.14	-0.746	-0.738	0.432
pt. source	0.062	-0.718	-0.693	0.617
Resolved
All	0.69	-0.850	-0.843	0.434
no SDSS	0.39	-0.895	-0.891	0.418
galaxy	0.19	-0.808	-0.803	0.386
pt. source	0.11	-0.737	-0.727	0.571
Compact
All	0.98	-0.715	-0.686	0.823
no SDSS	0.45	-0.842	-0.816	0.522
galaxy	0.23	-0.715	-0.674	0.686
pt. source	0.29	-0.297	-0.286	1.030

Table 6: The Sky Density, Mean, Median, and FWHM of α 9220 Histograms for the Data Samples Shown in Figure 14 and Table 5

Subclass	deg^-2	Mean	Median	FWHM
Complex
All	1.30	-0.802	-0.798	0.323
no SDSS	1.10	-0.813	-0.813	0.304
galaxy	0.14	-0.677	-0.674	0.323
pt. source	0.062	-0.740	-0.726	0.392
Resolved
All	0.69	-0.785	-0.787	0.334
no SDSS	0.39	-0.826	-0.836	0.316
galaxy	0.19	-0.722	-0.723	0.302
pt. source	0.11	-0.733	-0.725	0.379
Compact
All	0.98	-0.653	-0.584	0.646
no SDSS	0.45	-0.750	-0.705	0.444
galaxy	0.23	-0.609	-0.572	0.585
pt. source	0.29	-0.286	-0.244	1.060

If you use this catalog in your research, we would greatly appreciate it if you add a link to this site and a reference to Kimball & Ivezić 2008, AJ, 136, 684 in your publications.

   
   Amy E Kimball
   CSIRO Astronomy & Space Science
   PO Box 76
   Epping, NSW 1710
   Australia

   Željko Ivezić
   Department of Astronomy
   Box 351580, U.W.
   Seattle, WA   98195-1580
   USA

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