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tokens: Distances for each of these endpoints are reported explicitly, as well as the stream width. A5 Hermus We base our endpoints for the Hermus stellar stream on the galstreams footprint, which is based on the discovery paper (Grillmair 2014 ). One endpoint is computed using the galstreams algorithm, while the other does not match with an end of the stream and is identified separately. Distances for each of these endpoints are reported explicitly in Grillmair ( 2014 ), as well as the stream width. A6 Hyllus We base our endpoints for the Hyllus stellar stream on the galstreams footprint, which is based on the discovery paper (Grillmair 2014 ). Both endpoints computed using the galstreams algorithm do not match with the ends of the stream footprint and were identified separately. Distances for each of these endpoints are reported explicitly in Grillmair ( 2014 ), as well as the stream width. A7 Kshir Discovered using Gaia DR2 and confirmed spectroscopically by Malhan et al. ( 2019 ), the Kshir stream is distinct from but highly correlated in phase space with GD-1. We use two spectroscopic member stars as anchor points, corresponding to the highest φ 1 overall and the lowest φ 1 star from SDSS. These stars were chosen due to how close they are to the best-fitting orbit of Kshir and their high separation from each other. We assume both anchors are at the uncertainty-weighted distance of the stream (10 kpc) with ±1 kpc uncertainty, while the angular uncertainties are both assumed to be 0.5 deg. A8 Kwando We base our endpoints for the Kwando stellar stream on the galstreams footprint, which is based on the discovery paper (Grillmair 2014 ). Both endpoints computed using the galstreams algorithm do not match with the ends of the stream footprint and were identified separately. Grillmair ( 2017b ) reports the FWHM of the stream as 22 arcmin (Gaussian σ = 0.16 deg) and a physical width of 130 pc, corresponding to a heliocentric distance of 20.3 kpc. We assume both anchor points are at this distance and that the distance uncertainty is 20 per cent. A9 Magellanic Stream While the Magellanic Stream has been studied with great detail in recent years (Nidever, Majewski Butler Burton 2008 ; Nidever et al. 2010 ), its sheer size and complexity does not easily lend to being described by anchor points. We opt for the anchor points adopted by Pawlowski et al. ( 2012 ), which correspond to overdensities identified by Brüns et al. ( 2005 ). We adopt the same 55 kpc distance for both anchor points, with a 20 per cent distance uncertainty and an angular uncertainty of 2 deg. A10 Murrumbidgee We base our endpoints for the Murrumbidgee stellar stream on the galstreams footprint, which is based on the discovery paper (Grillmair 2014 ). Both endpoints computed using the galstreams algorithm do not match with the ends of the stream footprint and were identified separately. Grillmair ( 2017b ) quotes a heliocentric distance of 20 kpc. We assume both anchor points are at this