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Table 3

Simulation results.

Instantaneous (Gradual) Ram Pressure Stripping
Distance <1 Mpc <350 kpc <100 kpc <50 kpc
Companiona 36% (36%) 33% (34%) 22% (28%) 14% (24%)
Companionb 31% (31%) 21% (21%) 8.2% (8.2%) 4.7% (4.8%)
Companionc 26% (25%) 14% (13%) 4% (3.6%) 2.2% (1.7%)
Bright companiond 10% (9%) 2.4% (2%) 0.3% (0.25%) 0.1% (0.1%)
MH2 e 93% (93%) 69% (71%) 35% (39%) 24% (30%)
MHI e 94% (95%) 73% (75%) 37% (41%) 26% (32%)
SFR e 96% (96%) 78% (79%) 40% (43%) 28% (33%)
Quasar–companion galaxy systems with SFRintegrated> 500 M⊙ yr-1
M H2 f 100% (100%) 95% (98%) 72% (72%) 67% (67%)
M HI f 100% (100%) 88% (91%) 40% (67%) 35% (67%)
SFR f 100% (100%) 100% (100%) 100% (100%) 100% (100%)

Notes.

(a)

Percentage of quasars (LBj > 1044.5 erg/s) that have companion galaxies with M⋆ > 108M⊙.

(b)

Percentage of quasars (LBj > 1044.5 erg/s) that have companion galaxies with M⋆ > 109M⊙.

(c)

Percentage of quasars (LBj > 1044.5 erg/s) that have companion galaxies with M⋆ > 1010M⊙.

(d)

Percentage of quasars (LBj > 1044.5 erg/s) that have bright companion galaxies (SFR > 100 M⊙ yr-1).

(e)

Percentage of quasar–companion galaxy pairs where the H2 mass, HI mass and the SFR of the quasar host is smaller than that of the companion galaxies. Here the rates are calculated from the sample of quasar–companion galaxy pairs at the given spherical aperture.

(f)

The same as in (e) but in case of quasar–companion galaxy pairs that have an integrated SFR > 500 M⊙ yr-1 inside the aperture.

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