We appreciate the interest in the paper, but we understand the referee had some questions. We believe those can be addressed in a revised version.

The proposed revised version will follow the referee’s last suggestion in point 8 to not include the Ulysses and CCMC modelling (section 3, pp.15-23, subsections 3.1, 3.3, 3.4 and 3.5, Ulysses aspects in 3.2), keeping the near-ecliptic length-scale analysis of 3.2 only.

Thus, the revised paper will concentrate on the connections between the near-ecliptic in-situ observations. We will change the title to be “Longitudinally Spaced Observations of Magnetic Cloud Like Structure Embedded in a Co-rotating Interaction Region”. The abstract and some of the texts in the Introduction and Conclusion will also be shortened to focus on the comparison of observations at different longitudes near the ecliptic, which demonstrates the progression of the interaction between a Corotating Interaction Region and a Magnetic Cloud Like-structure from West to East.

As noted by the referee, the word ‘origins’ in the title was confusing. It was not necessarily to be understood as ‘solar origins’, while in Section 3 of the manuscript, we introduced the word ‘origins’ to mean solar origins. This is what may have been a misunderstanding. In the title we wanted to emphasise the interpretation of the observations with the word ‘The origins of’ in the title attached to the rest of the sentence containing the interpretation starting with ‘as’ from the analysis conducted in the paper. To avoid such confusion and with most of the section 3 removed, the new proposed title will be more appropriate.

Most of the points made by the referee (1,2,3,5 and 6) correspond to aspects of Section 3, and despite the interest in exploring this difficult event and the section 3 inviting discussions, we accept the limitations and are removing these parts.

We thus address the remaining relevant aspects in points 4, 7 and 8, not pertaining to Section 3.

1. For context, we will include an EUV image (and/or possibly a Carrington map) of the Sun to show the relevant coronal holes. Travelling the distance of 1 AU with the High Speed Stream speed of about 600 km/s indicates that the relevant coronal hole plasma parcel for the in-situ observations will be seen 2.9 days earlier on 1^st of July 2007.

1. The in-situ measurements are consistent with one or more structures developing between spacecraft. We will make sure the text is not misleading as we did not intend to say that they are strictly the same structure. However, we will present more discussions and include relevant literature. The longitudinal extent of blobs is likely to vary according to their size. Table 5 in our manuscript shows the length-scales of the MC(L) at the different near-ecliptic spacecraft, which are 0.07 AU at OMNI, 0.1 AU at ST-B and 0.12 AU at ST-A. The Y-GSE distances between ST-A and Earth and Earth and ST-B are about 0.17 AU and 0.14 AU, respectively. Magnetic discontinuities in the HCS surroundings are more likely to be aligned with the HCS and to have similar longitudinal extents as the HCS, as observed by Foullon et al. 2009 Sol Phys 259, with ST-A and ST-B separated by nearly 0.8 AU in the Y GSE direction. We will also refer to more recent works by Sanchez-Diaz et al. 2017 ApJ 851 32, Sanchez-Diaz et al. 2017 ApJL 835 L7 and Lavraud et al. 2020 ApJL 894 L19.

1. Fig. 6 shows the different structures already represented in the various spacecraft. The referee proposed a different launch date for the transients, with a speed of the transient of 194km/s. This speed is not consistent and rather low compared with the in-situ measurements of 330-444 km/s in the MCLs. Travelling the distance of 1AU with those speeds indicates possible formation/launch of the blob plasma at the Sun 3.9 to 5.3 days earlier on 29-30 June 2007. We will investigate adding an image of a blob around those dates in the HI data (similar but in place of Figure 8).