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tokens: product. We recommend not using the unofficial LAB HEALPix map any longer. 6.2. Spectral data The full spectral data will be provided for download in FITS binary table format on a HEALPix grid (nside-1024, Galactic coordinates are used for indexing). Because the EBHIS Milky Way spectral data set has a size of about 50 GByte, we split it into smaller chunks, namely into the 192 HEALPix pixels of the nside-4 tessellation. Because EBHIS is only available for declinations above , not all of the nside-4 pixels contain data, and these are therefore omitted. Additionally, smaller spectral data cubes of size are available for download in FITS image format. 7. Summary We presented the first data release of the Effelsberg-Bonn H i Survey (EBHIS), elaborated on the recent changes to the data processing software and techniques compared to Winkel et al. (2010) , and studied the quality of the resulting data products in great detail. EBHIS is a 21-cm H i line survey of the sky north of , comprising full spatial sampling and high sensitivity. At full spectral resolution of , EBHIS has an average noise level of . Its angular resolution is . About 1000 h of observing time with the Effelsberg 100-m telescope were spent until the completion of the first coverage that forms the basis for the first data release. Owing to the large bandwidth of 100 MHz, not only is the Milky Way emission covered in EBHIS, but also H i in the Local Volume out to a redshift of . The presented data products comprise the Milky Way emission. The analysis of the extragalactic part of the survey will be published elsewhere. EBHIS was designed to replace the northern-hemisphere portion of the important Leiden/Argentine/Bonn Survey (LAB; Kalberla et al. 2005 ), which has about a factor of 4 lower angular resolution and severely suffers from the insufficient spatial sampling (beam-by-beam only; compare Kerp et al. 2011 , e.g., their Fig. 7). Great effort went into developing new data reduction techniques, including but not limited to software radio-frequency-interference mitigation, a frequency-dependent flux-density calibration scheme, and robust baseline estimation in the 2D time-frequency domain. Furthermore, the very successful stray-radiation prediction algorithms, which were also employed for the LAB and Galactic All-Sky Survey (GASS; McClure-Griffiths et al. 2009 ; Kalberla et al. 2010 ; Kalberla Haud 2015 ), have been adapted to the Effelsberg telescope. We carefully assessed the data quality of the EBHIS spectra and inferred column densities. Our investigation revealed a mismatch in intensity calibration of GASS with respect to EBHIS and LAB, which led to a revised calibration scale in the third data release of GASS ( Kalberla Haud 2015 ). EBHIS and LAB show a near-perfect one-to-one relation in column densities and brightness temperatures. From a comparison of EBHIS and LAB, and from the overlaps of the EBHIS fields themselves, we estimated the uncertainties of the EBHIS column